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FRR Document - Louisiana Space Consortium

1. asisten edes ae VEGA SB Mund rate DO die 130 UD rcc CD Mae 131 28 Physical characteristio S co E Do 131 20 Waveform prOCeSSES isi eene aset cere ec ebay lain exeun aia cae istud 132 Velatile stored eo roe series qme see RUE NM REN 132 SAO pion TEE Orme oti iata seat ht Ge Dale ota Sa a alu 132 32 Hard 6opy capabDiliHle S sce cre ne o e vete n dette a esa enews a 132 SRM Tela unire REPRINT E 133 34 bnyironmental aud safety aone eco aem exce Pda deep qve iilius 133 on Risk likelihood tabl Car sea air evo ose nnde nata Mates pisa rama uude tus 134 BO RISK MAIX eco Queen E NE 135 37 BRISK SOIUttQns eo fa esas ted edite ctus ene tede i er bee e RN 137 Team CajunSat viii FRR v3 0 1 0 Document Purpose This document describes the critical design for the Cosmic Ray experiment by Team CajunSat for the ACES Program It fulfills part of the ACES Program requirements for the Flight Readiness Review FRR to be held May 9 2005 1 1 Document Scope This FRR document specifies the scientific purpose and requirements for the Cosmic Ray experiment and provides a guideline for the development operation and cost of this payload under the ACES Program The document includes details of the payload design fabrication integration testing flight operation and data
2. addrh CR block info for count storage 0 addrh addrh 1 WRITE 1 addrh FREQOUT 4 100 300 test beep for varification of operation ENDIF occurs about every 4 minutes IF nexttemp gt 256 THEN updates msb for temp storage addrblock addrblock 1 nexttemp 0 WRITE 3 addrblock ENDIF IF addrh gt 7 THEN after 1 2 an hour HIGH heater ENDIF turn on heater LOOP The following program is designed to convert the bit data from the EEPROM to temperature in C It will be used for us to make sure that our payload stayed within the correct operating temperature ISSTAMP BS2p ISPBASIC 2 51 This program is made to read temp data off eeprom 2 SDA PIN 0 I2C SDA pin SCL PIN SDA 1 addrlow VAR Word internal address addrhigh VAR Word internal address value VAR Byte value to write result VAR Byte array for returned value Team CajunSat 6l FRR v3 0 Read From EEPROM DEBUG CR Reading CR FOR addrhigh 0 TO 255 FOR addrlow 0 TO 255 I2CIN SDA A1 addrhigh addrlow tempout addrlow addrlow 1 PAUSE 10 I2CIN sda A1 addrhigh addrlow tempin addrlow addrlow 1 PAUSE 10 DEBUG DEC addrlow CR DEBUG DEC tempin inside CR DEBUG DEC tempout outside CR NEXT NEXT PAUSE 100 DEBUG CR locations read END Team CajunSat 62 FRR v3 0 This program is designed to clear the data off the EEPROMS This program clears out the eeproms on the balloon project b
3. 11 EDS CTVE 0 800Amps AC 74x64cm 135cm 15 0cm 28cm Tm 29028 hy 85m Le TMC6 HC Stainless Stee Temp Probe 4 20 mA cable Stainless Steel temperature probe rucc Range 0 to 20 1 mA x 10 2 cm 4 food grade stainless steel probe with pointed tip 0 3 cm 0 12 mS zim reading Resolution wH6 0 4 of full scale Range 40 to 100 C 40 to 212 F in air or water w U12 0 03 of full scale Accuracy w H8 0 5 at 20 C 0 9 at 68 F 45 7 cm 187 cable with 8 9 3 5 tinned Accuracy w12 025 at 20 C 20 45 at 68 F wire leads Resolution w H8 0 41 at 20 C 0 7 at 68 F 4 20mA Cable Resolution w U12 0 03 at 20 C 0 05 at 68 F Voltage input cable casc2ssteco Response time moving 1 m sec 2 2 mph 1 8 m 6 cable with 1 27 cm 0 5 tinned braided amp 3 min typical to 90 wire leads in stirred water 15 sec typical to 90 For voltage input specifications refer to the ifications of the model you will be usi gt Additional sensors cables on pg 8 0 2 5 DC Cable Figure 11 8 continued This shows the all the data on the HOBO http www onsetcomp com Products Product_Pages pdfs h08 00x Ox pdf Team CajunSat 96 FRR v3 0 The following graphs are for box design We currently do not have any double box design test This will be done latter this wee
4. Ankle 1 particle km year 10 10 40 107 10 10 109 19 1078 10 1020 19 Energy eV Figure 3 3 This graph shows the flux of cosmic rays bombarding Earth as a function of their energy per particle Researchers believe cosmic rays with energies less than 3x10P eV come from supernova explosions The origin of cosmic rays greater than 10 remains a mystery http www firstscience com site articles balloon asp Team CajunSat 6 FRR v3 0 15 Protons 9 100 Eev Protons 1 Zev Fe 100 EeV log Magnetic field gauss I tw 9 3 6 9 12 15 18 21 L au 1 pe 1 1 Mpc log size km Figure 3 4 Hillas Plot Red green and dotted lines show the relation between the magnetic field and the size of an accelerator Once energy and charge of the accelerated particle are fixed Astrophysics objects placed above a line are candidate sites for acceleration http etd adm unipi it theses available etd 06 1 42004 2154 16 unrestricted ch1 pdf Team CajunSat 7 FRR v3 0 bhw electrons positrons This is a computer simulation of the primary cosmic rays interacting with the atmosphere cyan photons http www th physik uni frankfurt de drescher CASSIM red neutrons orange protons gray mesons green muons Team CajunSat 8 FRR v3 0 Figure 3 5 B This is a computer simulation of the primary cosmic rays interacting with the atmosphere cyan phot
5. Power Budget Component Voltage Current Power BalloonSAT and 9V Low 0 04 A Low 0 36 W Geiger Counter High 0 06 A High 0 54 W Batteries 9V 1 8 11 7 W Table 4 1 This is our power budget table for the flight There are two lithium batteries being used One is for the Geiger counter and the other one is for the BalloonSAT and heater The power supply of the payload will consist of three 9V lithium batteries One battery will be supply the Geiger counter and the Interface board while the other battery will provide power to the other electrical units The complete interfacing design can be viewed in figures 4 3 4 4 and 4 5 There will be four main electrical components heating circuits described thoroughly in section 4 4 and figures 4 7a and 4 7b This circuit will consist of a 0 5 W ceramic resistor and there will be two of them located within the payload Temperature data will be stored with the BASIC stamp and its memory on the BalloonSAT board The final two components are the Geiger counter and the Interface Board which will be interfaced together reference to figure 4 6 for the interfacing schematics This interfacing is described as follows The CD4040 is used to count the Geiger ticks The clock input is connected to the middle of two series 100 K resistors One of the resistors is connected to ground and the other is connected to pin four of IC U1 the CD40106 or 74C14 on the Geiger counter The Stamp will be powered from
6. 1 1 1 Document SCODE up ees oii eio e Rea 1 1 2 Change Control and Update 2 etr eer deiecit set 1 2 0 tenes xe eas 1 DA Mission OBIGet Ve S au eco d eed di Rak dU d 2 3 T Science esci e edv epi ideis spleen ea tns DU a day a tuns d o Pe Ce erg 2 ERU Grecia AVG oer HD 3 221 2 MUONS ones oe ue m Lu dU LU M ME IL m T 17 3 1 3 Non Vettieal vire ii coa poer vts eds 18 Sd d Interaction Depth o Ud iu ep Hope End uci us 19 2d 5 Sl nt sio t m d de 22 Sc PC HIN CAL Roster ete tr t eaves Ree oa 22 4 0 1 sostenute e ire a e Paco Leon dun 25 4 1 Principle of Operation ecce nce erect die luxe bue tid ete aide Lacs uds 30 d SVeter ICS TOT a cedes ea er ec aq eiae i bs uM eae fedus Io 33 4 3 Bleetriedl Design os n a 34 4 3 Software DESI ON ahs iuis tede tese tr eret ere dede d t 36 AA Thermal Design Iota dva xd iau teo Eabb Pop iu un Puget na biu 37 4 5 Mechanical DeSIri uu e og oi b SECO T s c E E E E EE E E ER x 3
7. Cosmic Ray Counts versus Altitude e 8 o Rate Counts 7 minute z ASCENT DESCENT a ca T T T T T 0 10 20 an 40 60 To a0 90 100 Altitude thousands of feet Figure 3 11 Expected results according to FRED experiment performed by LSU team e Ascending Descending Counts per Minute Q e a Q Hess flight 17 000 ft 5 400 200 0 20 40 60 80 100 Kilofeet above Sea Level Figure 3 12 This is another cosmic ray experiment It was performed on FLIGHT BORO109A by the Montana High Altitude balloon program http spacegrant montana edu borealis missions BOR0109A index php Team CajunSat 24 FRR v3 0 4 0 Payload Design Foam core NS L K 15 cm i 15 bra 4 15 Figure 4 1 This is the outer box which will house our inner box This box will also have a switch on the outside running from the BalloonSAT to outside the box This is for us to be able to turn on the BalloonSAT just before launch to conserve battery power Team CajunSat 25 FRR v3 0 Foam core Heaters E Batteries B BalloonSAT Geiger counter Figure 4 2 Diagram of our inner box 4 1 1 Geiger Counter The first thing that we need to calculate the flux is the amount of particles counts at a given altitude To get this we will use a Geiger counter which according to Webster is an instrument for detecting the presence and intensity of radiatio
8. Team CajunSat 54 FRR v3 0 Figure 6 11 This is the gamma sensitivity curve for the Geiger tube http www Indinc com gm alpha draw sen7232 gif Figure 6 12 Picture of the Geiger tube http www Indinc com gm alpha draw pic7232 jpg Geiger Plateau To find the Geiger plateau of this device we followed the directions of The Geiger Counter Experiment using a Cobalt 60 source We did each measurement of each distance twice and then took an average before finding the plateau The data and Geiger plateau can be found in Table 3 4 and Figure 3 12 We have concluded that the optimal voltage for the LND 7323 counter is 725 V We are unable to change the voltage of the K2645 Geiger counter therefore we will not be performing this experiment on the K2645 This was only done to make sure that our calibration Geiger counter is running at the correct voltage Team CajunSat 55 FRR v3 0 Close Distance Counts Volts Run 1 Run 2 800 896 987 775 896 891 750 916 864 725 866 873 700 840 848 675 859 766 650 650 732 625 0 0 Table 3 4 A This is the data for our close distance which was the first slot Team CajunSat Far Distance Counts Average Counts Volts Close Average Far Average 800 941 5 332 775 893 5 271 750 890 252 725 869 5 250 700 844 245 5 675 812 5 240 5 650 691 200 5 625 0 0 Table 3 4 C Th
9. WBS etes eot bd risas use votaste ua e na iid 74 Plam det ec elo t b ea Pei buen 75 9 3 Timeline and TONGS red tese Teen Wet a tet PUE UM 76 10 0 Master BU Sets naa petrae duces asa aUe MANI 77 S ee S rt bec brc hn 78 10 2 Material Acquisition Plan eo aere re is tete 79 11 0 Risk Management and s ihe epe erbe tO eese ated auia s 79 testing esce erat toco tatit eds d tenda etes nde e e euer 87 11 2 Cold testing iro xiu 98 113 Vacuum TESTIS aes ea ee See Caio E nee cla NN d ELA 99 11 4 Testing of RE CNG deos eie e e Dile adden aai 99 11 5 Complete system test of all equipment and in all conditions esses 133 12 0 GOSS acest totae tete D ere E Ra Tace Ghi ome la deka e pdt ae Era i a ale d 136 Team CajunSat FRR v3 0 LIST OF FIGURES 1 Stopping material of oie eerie et e bete tbe as 3 2x Victor Hess Pet iecur pri res iode ite tendi ub abogada dabas 5 3 Flux OF Cosmic ob ode D ens rated D ede de M put read hub 7 d STARA Gist 38660 M MC LER AM CC 8 2 COSIIGSIIOWSE ese mee se ial itae 9 6 Geiger NT I 19 T Gei
10. e Integrated external calibration weights e Unique durable design for all applications e Applications include Counting Percent Weighing Totaling Display Hold Specific Gravity Mass unit conversion e 14 Mass unit conversions g oz lbs lbs oz dwt ozt grains Newton carats Taels HK Taiwan Singapore China user defined Optional RS 232 or USB interface kit field installable Parts counting with selectable reference sample 1 100 Included AC adapter External one button calibration with 3 weight options Lock down capability Two year manufacturer warranty Team CajunSat 42 FRR v3 0 Figure 4 9 Picture of the scale we are using http www acculab com products Figure 4 10 Picture of us actually weighing the box Team CajunSat 43 FRR v3 0 Calibrations for Balance To calibrate the weight and get the error we did the following 1 UT x UN Put our balance on a level surface Zero it out Use Fisher 540300 Brass weight set of various weights Use 2 measurements of the weights to get an average error The following is a list of the error Weight Error 200 g 20 014 g 100 g 0 019 g 050 g 0 006 g 020 g 0 004 g Table 4 2 Average area of the weights Figure 4 11 This one 200 g weight being used to calculate the error of the balance Measuring procedures are as follows If the weight is less than 300 g we will use the VIC 303 0 001 g Precision Balance and the follo
11. ied Ed Pax ids 57 Be Slant Depthangles a de cate t eee Mrs EA dine 57 9 Requirements of MAA WATS eoi bep ea Re ua dengan inde asc tba Mab 72 IG Power Budget x ce terrea dtr te et Pea pee err NEA 80 IH Balance HOLD oem boe taste vdidm at ra M Li 82 12 Weight Budget e oe se o dS eue deum RE Ue aa aa 87 13 Hardware fabrication and testing cett eere dae 93 14 Organization n ve re rA Io av EE Idas 100 I5 Work Dreakdo3vn str c tfe Sassi todo depen 2 103 eeepc eta E aeu SUE an ohare D LUE 104 17 Mater aqu testas beer teste eod lest etes olx asd dd Paese oe axial 106 18 Purchase recordi o evite oce tito tona enter qu ree utere Seed em bred 108 19 Specifications for Scientific workshop 119 ratius A or hoes lcs 122 21 Voltage Sensor Specifications s a eri te 122 22 1pial Acquisition Systeri cube iau does aput tes ban pet essa qua tita bU E ted adiu 129 23 Calibration d AHg es cuoco coo oo Do pde beide edd Op 129 24 Time base systems ceca diete A Sod epe esten luisse tame ust E ea Lu 129 DAP Trigger SVSLOM IR E A 130 26 DISDIdy
12. p ad ALKALINE E CARBON ZINC 5 0 10 15 20 25 Service Life Hours Voltage V Typical Discharge vs Temperature 90022 Continuous Discharge 10 20 30 40 50 70 80 90 100 110 120 130 Service Life Hours Typical 3000 27 mA Continuous Discharge at Room Temperature 10 15 20 25 Service Life Hours 30 35 40 Team CajunSat Safety Less than 2 grams of lithium no restrictions on transport MSDS available separately Recognized under the Component Program of Underwriters Laboratories Inc W Typical Continuous Discharge Capacity 01 02 03 04 05 06 07 08 09 Battery Capacity Amp hours 10 11 12 13 WT Short Circuit Test Temperature vs Current vs Time Temperature C esssscgsas Typical 600 120 mA Continuous Discharge at Room Temperature 1 Service Life Hours Newark NY 1 315 332 7100 Fax 1 315 331 7800 Abingdon England 44 0 1235 542600 Fax 44 0 1235 535766 2002 Ultralite Batteries Inc www ultralifebatteries com All specifications subject to change without notice The information contained herein is for reference only and does not constitute a warranty of performance Apr 2 02 UBI 3002 rev 41 FRR v3 0 The scale we are using is VIC 303 0 001g Precision Balance with the following features e 4 models with milligram readability e Protective flip down and removable plastic cover for shipping protection and allows stackable storage
13. which has only scheduled dates for the preparation for FRR and flight operations Team CajunSat 72 FRR v3 0 9 1 Work Breakdown Structure WBS Section 9 1 Work Breakdown Structure WBS and Staffing Plan I Lithium battery load check Ross II Design heating circuit Jasmine Donald 1 Build heating circuit Ross 2 Test heating circuit Ross III Build Geiger counter kit Jasmine Donald 1 Geiger counter rate check Ross 2 Geiger counter accuracy check Ross 3 Geiger counter environmental check Ross IV Design interface board Jasmine Donald 1 Build interface board Jasmine Donald V Build a system mock up for testing Robert 1 Interface communication test Jasmine Robert Ross Donald 2 Interface baseline check Jasmine Robert Ross Donald VI Prepare CDR documents Mikhail VII Design structural layout Jasmine Donald VIII Build a system mock up for testing Robert 1 System mock up shock test Jasmine Robert Ross Donald 2 System mockup environmental check without heater Jasmine Robert Ross Donald 3 System mockup environmental check with heater Jasmine Robert Ross Donald IX Build final payload Robert 1 Final system checks Jasmine Robert Ross Donald X Prepare FRR documents Jasmine Robert Ross Donald Team CajunSat 73 FRR v3 0 9 2 Staffing Plan Task Name Start Finish Duration BBL EEE E EE REA Cae eds H Desi heaing ciut g B
14. 3 5 G This is a computer simulation of the primary cosmic rays interacting with the atmosphere http www th physik uni frankfurt de drescher CASSIM orange protons gray mesons green muons FRR v3 0 14 Team CajunSat Figure 3 5 H This is a horizontal view of the secondary cosmic ray shower ih http www th physik uni frankfurt de drescher CASSIM cyan photons red neutrons blue electrons positrons orange protons gray mesons green muons Team CajunSat 15 FRR v3 0 Figure 3 51 This is a vertical view of the secondary cosmic ray shower blue electrons positrons http www th physik uni frankfurt de drescher CASSIM cyan photons red neutrons orange protons gray mesons green muons Team CajunSat 16 FRR v3 0 This interaction of primary cosmic rays causes a graph as in Figure 3 6 The reason for the peak has to do with the interaction length which is given by the following muon example Aititude in km 2 8 10 min Variation of comic rays Wi aide Counting rate M i BOO GOO 400 206 o Atmospheric prossuno in mmtig Figure 3 6 This shows the theoretical curve of the flux with respect to altitude 3 1 2 Muons Muons are the most numerous charged particles at sea level In other words muons must lose energy by ionization because it is charged There is no way around this because as it passes through matter it interacts with the electric fields which knocks loo
15. CajunSat 29 FRR v3 0 4 1 Principle of Operation The Geiger Muller Counter will measure the flux of cosmic rays in counts per minute This counter will be interfaced with the BASIC Stamp sending data to the EEPROM of the BASIC stamp Temperature measurements will be collected throughout flight and stored into the BASIC stamp These measurements will be used to determine that the electronics remained in operating temperature range 20 C 70 C To maintain this temperature there will be two heating circuits inside the payload as noted in the above figure 4 1 If a particular section of collected data seems inaccurate we can reference our temperature data for a plausible cause of the inaccuracy After flight using pre tested software the data will be dumped from the EEPROM of the BASIC Stamp The goal of our payload is to combine the collected data from flight and the tracking team s data to produce a final graph of the intensity of cosmic rays in flux with respect to altitude as described in section 3 0 Requirements Hardware Internal temperature must remain at a One heating circuit and a double box minimum of 20 C for proper functioning design will be used to ensure that the of electrical devices temperature does not go below 20 C To determine if electronics stayed in Thermistors on the BalloonSAT will be necessary temperature range Temperature used to make sure that we have maintained readings are needed to be collected
16. Gain Accuracy 2 Vertical Resolution 8 Bits 256 levels over 10 24 vertical divisions Acquisition Modes Sample Envelope Average High frequency and random glitch capture Captures glitches as narrow as 10 ns using acquisition hardware at all time div settings between Peak Detect 25 us div and 5 s div inclusive Table 11 4 This shows the characteristics of the signal acquisition system of our oscilloscope http www tek com Measurement cgi bin framed pl Document Measurement Products catalog tds300 specs html amp FrameSet oscilloscopes Volts Div Setting Offset Range 2 99 5 mV div 1V 100 995 mV div 10 V 1 10 V div 100 V Table 11 5 This shows Calibrated Offset Ranges of our oscilloscope Time Base System Main and Delayed Time Division Range 5 ns to 5 s div Record Length 1000 sample points per channel Horizontal accuracy 0 0196 Roll Mode 0 1 s div and shower when Auto Trigger Mode is selected Table 11 5 This shows the time base system of our oscilloscope http www tek com Measurement cgi bin framed pl Document Measurement Products catalog tds300 specs html amp FrameSet oscilloscopes Team CajunSat 100 FRR v3 0 Trigger System Only Trigger types Edge Video Trigger Modes Auto Normal Trigger Inputs CH1 CH2 Line External Triggers on Field 1 Field 2 Any Field noninterlaced systems or Lines Video Type from Sync negative
17. a correct operating temperature Data needs to be stored from Geiger Counter in order to analyze results in the BASIC Stamp is connected to end also a timing device is necessary to BalloonSAT which has a timing circuit keep accurate accounts of the time in which already built in is inside payload and two the data from the Geiger counter came so it EEPROM s for storage of the Geiger can match with the corresponding Counter and temperature readings temperature reading Fig 4 2 Table of the flow from Requirements to Hardware 4 1 2 Flux The second thing we need to know to calculate the flux is the surface area of the detector This turns out to be really simple because the particles are traveling near the speed of light making the Geiger tube a stationary target for the particles see Figure 3 18 Also for the most part the Geiger counter will only rotation along the xy axis with very little motion around the z axis This Team CajunSat 30 FRR v3 0 means all we need to do is measure the length and width of the active area of the detector We did this by using a vernier caliper to get very accurate 0 05 mm measurement and then substituted the results into the following equation Area length width Beta Particle Beta Particle Beta Particie Y Beta Particle T y 49 49 Y 4 49 Particle T Beta Particle Beta Particle 4 Beta Particle Y 49 4 7 Beta Particle Y 49 Beta Particle i 4 Bet
18. analysis In addition project management timelines work breakdown expenditures and risk management is discussed Finally the designs and plans presented here will be finalized at the time when the ACES Program Office approves this Flight Readiness Review FRR 1 2 Change Control and Update Procedures Changes to this FRR document shall only be made after approval by designated representatives from Team CajunSat and the LaACES Program Office Document change requests should be sent to Team members and the LaACES Program Office 2 0 Reference Documents 1 Mewaldt R A Cosmic Rays California Institute of Technology Macmillan Encyclopedia of Physics 1996 http www srl caltech edu personnel dick cos_encyc html 2 Introduction to Ionizing Radiation and Low level Radioactive Materials Dr William Andrew Hollerman CHMM 3 Cosmic Rays NASA http imagine gsfc nasa gov docs science know_12 cosmic_rays html http helios gsfc nasa gov cosmic html http imagine gsfc nasa gov docs science know ll cosmic rays html 4 Stanton Noel Introduction to Cosmic Rays July 9 2003 http www phys ksu edu evt Quarknet Docs cosmic_ray_intro pdf 5 http hyperphysics phy astr gsu edu hbase astro cosmic html 6 NASA COSMICOPIA http helios gsfc nasa gov qa cr html 7 Uranium Information Centre Ltd Nuclear Electricity 7th edition 2003 http www uic com au neApl htm 8 FRED PDR document http atic phys lsu edu aces Teams 2002 2003 FLU
19. and off heater addr VAR Word Isb byte for gm count storage addrh VAR Word msb byte for gm count storage beeper PIN 4 buzzer pin main LOW heater make sure heater is off FREQOUT 4 1000 300 produce tone to demostrate proper operation READ 3 addrblock set start of mem address READ 2 nexttemp i READ 1 addrh i READ 0 addrl DO LOW tempcs SHIFTOUT tempda tempcl LSBPOST ch1sel initiate adc0834 COUNT gmin 3484 gmcount read 1 sec of G M collisions DEBUG DEC gmcount LOWBYTE DEC addrh DEC addrl CR I2COUT eelda A0 addrh addrl gmcount HIGHBYTE store counts msb 8 addrl addrl 1 PAUSE 4 I2COUT eelda A0 addrh addrl gmcount LOWBYTE store counts Isb 8 addrl addrl 1 WRITE 0 addrl update mem location SHIFTIN tempda tempcl MSBPOST temp 9 read inside temp I2COUT ee2da A0 addrblock nexttemp temp store inside temp 1 DEBUG DEC temp CR this line for outputting temps while running HIGH tempcs LOW tempcs initiate adc0834 SHIFTOUT tempda tempcl LSBPOST ch2sel PAUSE 10 SHIFTIN tempda tempcl MSBPOST temp 9 read outside temp I2COUT ee2da A0 addrblock nexttemp temp store outside temp 1 DEBUG DEC temp CR this line for outputting temps WRITE 2 nexttemp while running Team CajunSat 60 FRR v3 0 HIGH tempcs IF addrl gt 255 THEN this section is for updating msb DEBUG DEC addrl
20. cm 0 20 Operating range 0 to 60 C 32 to 140 F Note Sensor tip and cable immersion in fresh water up to 50 122 F CTV A B C 0 to 40 C 32 to 104 F CTV D E for 7 year radiation shield recommended for use in sunlight Construction and operating environment Molded plastic housing for indoor use per UL508 All units have opening leg that snaps into place Narrow Range temperature sensor for H8 loggers 1 8 67 cable compatible w H8 and U12 extemal Range 0 to 44 C 32 10 110 F in air Leg on CTV D and E units is removable Accuracy w H8 0 4 at 20 C 0 7 at 68 F Note AC current sensors are not CE approved w U12 0 25 at 20 C 0 45 at 68 F Resolution w H8 0 2 at 20 C 0 3 at 68 F w U12 0 011 at 20 C 0 02 at 68 F Outer Outer Response time in ar moving 1 misec 2 2 mph Part Range Window Length Width Height pu ae CTVA 020AmpsAC 28 23 74cm 66cm 25cm n DCN mor 28 10 Sensor diameter 0 8 0 3 sensor Temperature Sensor CTVB 0 50 Amps 28x23cm 74cm 66cm 25cm eee 14x09 29 26 10 Note Do not use for more than 3 months total in water less than 30 CTVC 0 100 Amps AC 28x23cm 74cm 66cm 25cm 86 F or more than 1 month total in water over 30 C 86 F 0 0 e 26 10 CTV D 0 200AmpsAC 38x33cm 99cm 11 9cm 28cm rU ind 15x13 39 AT
21. cosmic html Vacuum testing procedures Seal the vacuum chamber without anything inside and then measure the amount of time that it took for the vacuum to go all the way down Then place the object you want to vacuum test inside and measure that time If it takes longer then there is some outguessing occurring Also observing the object inside and looking for fumes is something else that we try to do The final test is to take a close look at the object after it is finished with the vacuum test to see if there are any significant changes such as becoming brittle Cold testing procedures The first thing we do is get between 10 20 Ibs of dry ice at a U Haul place near campus Then we place the object in our cold chamber see Figure 11 18 B Next we put the dry ice around the object but not touching the object We then place temperature probes in the cold chamber to get Team CajunSat 58 FRR v3 0 the temperature of the objects environment and place either a HOBO or temperature probe inside with our object Finally we let in stay in that environment and observe the results Minimum operating temperature procedures To find the minimum operating temperature we do a cold test on the environment and see how the object performs as the temperature goes down When the object can no longer operate as it is designed to we record the minimum operating temperature and try to keep it within its operating limits Geiger counter test To test the Geiger
22. counter we will place a Cobalt 60 source at a certain distance and let it record the counts per minute We will also take another Geiger counter and do the same thing to it After both test are complete we will compare the results of the Geiger counters Integration After the heaters and Geiger counters are constructed and working properly we will connect them to the BalloonSAT When they are connected we will run tests to make sure that they function with the BalloonSAT and can store the data on the BalloonSAT The heaters must be able to be turned off and on as the temperature drops to below 0 C 6 3 Software Implementation and Verification The Basic stamp will run the following program This program is designed to get the counts temperature and turn on the heater if the temperature gets too cold inside SSTAMP BS2j SPBASIC 2 5 gmcount VAR Word gmin PIN 5 set geiger input pin eelda PIN 8 labels temp eeprom eelcs PIN eelda l chip enable pin ee2da PIN 0 labels temp eeprom ee2cs PIN ee2da l chip enable pin tempda PIN 13 adc8031 data pin tempcl PIN 14 adc0831 clock pin tempcs PIN 15 adc0831 chip enable pin chlsel CON 1110 adc0831 channel 1 constant ch2sel CON 1101 adc0831 channel 2 constant temp VAR Byte used for adc0831 data nexttemp VAR Word used for temp eeprom address Team CajunSat 59 FRR v3 0 addrblock VAR Word used for temp eeprom address heater PIN 7 used to turn on
23. expected to complete their sections according to schedule and work independently on their own time if necessary Any changes to payload or schedule will be voted on during group sessions This is needed so we will be able to determine potential budget or deadline issues The team leader will be responsible for overall project flow and will actively monitor the budget and progress Every team member is responsible for keeping accurate records on their respective sections and team record keeper will centralize the records as needed Any parts needed will be ordered by the graduate assistants or by project oversight Team CajunSat 69 FRR v3 0 8 1 Organization and Responsibilities Contact Information Dr William A Hollerman Noah Bergeron Mikhail Yevdokimov Robert Moore Ross Fontenot Jasmine Bulliard Donald Crouch Team CajunSat hollerman louisiana edu noah_bergeron hotmail com myevdokimov gmail com kazzatfu yahoo com rsfontenot Whotmail com jbb4462 louisiana edu ionace hotmail com 70 FRR v3 0 8 2 Configuration Management Plan Any changes to payload design are implemented according to following procedures Design Change Plan Change request posed during team meeting All members of team votes on change Budget monitor will assure change fits in budget and advise team leader Team leader will give final approval Record keeper will document relevant PDR CDR sections Un dec qaum 8 3 Interface Contr
24. from the EEPROM and display then counts in counts per minute We will then use EXCEL to calculate the flux J2C BSP This program outputs the data of the gm eeprom and displays the information by minute SSTAMP BS2p SPBASIC 2 5 SDA PIN 8 2C SDA pin SCL PIN SDA 1 addrlow VAR Word internal address addrhigh VAR Word internal address block VAR Nib block address in 24LC16 value VAR Byte value to write result VAR Byte array for returned value mincount VAR Word number of mem locations read MINtotal VAR Word number of counts minnum VAR Word number of minute being totalled Read From EEPROM minnum 0 mincount 0 mintotal 0 DEBUG CR Reading CR FOR addrhigh 0 TO 255 FOR addrlow 0 TO 255 mincount mincount 1 I2CIN SDA A1 addrhigh addrlow result mintotal mintotal result IF mincount 120 THEN mincount 0 minnum minnum 1 DEBUG DEC mintotal counts in minute MINnum CR mintotal 0 ENDIF NEXT NEXT PAUSE 100 DEBUG CR All locations read END Team CajunSat 65 FRR v3 0 This program erases all the data stored on the EEPROM SSTAMP BS2p SPBASIC 2 5 This program sets the eeprom memory locations to start at zero WRITE 0 0 WRITE 1 0 WRITE 2 0 WRITE 3 0 END We will calculate the dead time of our software once the flight is over The procedures for this are discussed in the dead time section Team CajunSat 66 FRR v3 0 6 4 Flight Cert
25. measures the current As this process occurs the gas ions are slowly building up around the outer wall of the probe which forms a sheath This reduces the potential and stops the cascade of secondary particles Once the cascade has ended the ions and electrons recombine to form the neutral gas atoms again This process called quenching and serves to reset the detector allowing it to detect another radioactive emission This cycle of the first ionization to the resetting is referred to as the dead time and is typically 100 to 300 microseconds To get a better picture of this see Figure 3 6 Reference 14 Another thing that we must figure out for the Geiger counter to operate effectively is the Geiger plateau If the voltage is too low the passage of radiation into the tube will not cause a voltage pulse The characteristic curve for any tube is obtained by graphing the counting rate verses the applied voltage This curve is shows in Figure 4 3 The counting rate C is the number of counts N registered by the tube divided by the counting time T The region where the number of counts is approximately linear and changes little with voltage is called the Geiger plateau To preserve the life of the tube the operating voltage is generally selected within the initial 1 3 of the plateau We will find this plateau for our calibration Geiger counter by placing a radioactive source and adjusting the voltage Afterwards we will graph our data and dete
26. of 20 C proper synchronization of all devices inside and outside of the payload Post flight Requirements GPS time latitude longitude and altitude to properly analyze our data Proper functioning of all interior devices Geiger Counter BalloonSAT in order to collect needed graphs and data 7 3 Data Acquisition and Analysis Plan The Velleman K2645 Geiger Muller Counter will be interfaced to the BASIC stamp allowing all data from the Geiger counter to be stored into the EEPROM of the BASIC Stamp as standard units of counts per minutes Post flight the data will be collected via computer and a pre written pre tested program will convert the units of counts per minute to flux refer to section 3 1 for details about these conversions Once we have collected all necessary data including GPS time latitude longitude and altitude from the tracking team Graphs will be acquired in order for comparison to expected results Error will be calculated between acquired results and expected results This error will be included in the final data analysis Team CajunSat 68 FRR v3 0 8 0 Project Management We will meet on Thursdays from 5 00 pm till 8 00 pm and on Fridays from 2 30 pm till 7 00 pm for group work These sessions are to discuss completed sections and decide on future workflow We will discuss any problems encountered and methods chosen to correct them Any additional group work periods are scheduled as needed All individuals will be
27. the most cost efficient These details are located in the above section 10 0 Testing supplies have been purchased multiple times during programs timeframe The biggest expense that we have encountered with testing supplies is dry ice which is 1 00 pound We used dry ice on a regular basis for our testing procedures of all of our components that are to go in the final payload According to Figure 10 2 testing supplies will take approximately 15 of our budget We have purchased some building supplies although more will be purchased when the time comes to build the final payload Building supplies mostly includes foam board aluminum tape glue epoxy and other small items these supplies take up approximately 10 of our budget Figure 10 2 The only other expenditure that we have not yet purchased is the heating coils used for marinating our payloads temperature around a minimum of 20 C Heating elements will only take up 2 of our budget according to Figure 10 2 We have 27 of our budget left over after accounting for all expected expenditures Therefore we will have more then enough left over budget to account for additional supplies we may need 10 2 Material Acquisition Plan Item Acquisition Order Need Date Date Baene Needed on multiple accounts throughout entire project Vacuum chamber Existing Supplies Nee ona regular Dasib for testing Dry Ice Purchased Purchased as needed for project Cold Chamber Existing S
28. to construct 20 00 purchased at local Geiger Muller Counter in the this portion of retail store Counter account it becomes our the payload primary user No wait time Ceramic resistors Ceramic resistors used for purchased at local 99 cents per Heating 10 00 heating payload retail store resistor at Radio Shack Most costly items were board N ee to build box Final ore Mem which is around Supplies pA PERAI WESS c to build final box and have spare for testing needs No wait time z Pry ipe was Foam board for designing most costly item purchased at local Testing cold chamber dry ice etc We regularly 75 00 retail store Supplies purchased dry ice for our testing Total Estimated 365 00 Cost Table 10 1 Budget Table Four suppliers for the V K2645 Geiger Muller Counter kit part N32VKK2645 were priced to be the most cost efficient with the budget The result of our research was as follows Team CajunSat 76 FRR v3 0 PogeeKits Electronic Kits and Tools 148 50 http www apogeekits com geiger_counter htm Gibson Tech Ed Inc 143 99 http www gibsonteched com vk2645 html Carl s Electronics Inc 179 95 http www electronickits com kit complete meas vek2645 htm Electronix Express 139 95 http www elexp com kit_2645 htm We determine to go with PogeeKits Electronic Kits and Tools The two suppliers with lower prices were sold out of the V K2645 which would have resu
29. uim t oli Bn E y 1 10 p R h 0 M count rate as a tunction of dose rate Figure 3 15 Graph of typical count rate as a function of dose rate from Cobalt 60 source This comes from the product manual Team CajunSat 48 FRR v3 0 Comparing the gamma sensitivity graphs of both Geiger counters we see that LND 7232 has a greater counts per second In fact it is approximately a factor of ten greater than the K2645 Geiger counter The reason for this is the LND 7232 is more sensitive to radiation and it has a larger detection area The way we will compare each Geiger counter is to measure the flux of each graph We also expect the LND 7232 Geiger counter to have a little higher flux rate compared to the K2645 counter The reason for this is because the LND 7232 counter has the ability to detect alpha particles while the K2645 cannot detect them We ran all of our runs inside therefore the walls stopped the alpha particles but it can still detect a larger amount of radiation making it a little more flux compared to the K2645 The two should still be very close however 6 0 Payload Construction Plan 6 0 1 Assembly of the Geiger Muller Counter K2645 Label Artnr Qty Description BUZI SV3 1 SOUNDER VELLEMAN 3 30VDC 8mA 12V LEADS CI 220J0C 1 ELCO PCB 220uF 16V C13 033 1K 1 33nF 1000V 14 7 47 1 MKH 0 047uF 250V C2 5110030 1 SIBATIT 100nF 63V C3 1 1000 1 MKH 1 100 C4 7M1 1 MKH InF 400V 5 12 7MK33 8 M
30. 00 C to 200 C less than 0 5 C full scale 0 2 C 10 mV linear platinum wire 8 pin DIN plug Team CajunSat 90 FRR v3 0 Table 11 1 This is the specifications of the RTD table http store pasco com pascostore showdetl cfm amp DID 9 amp Product_ID 51267 amp Detail 1 TERESA Ae SENSOA ATA Figure 11 2 This is a picture of the RTD temperature sensor http store pasco com pascostore showdetl cfm amp DID 9 amp Product_ID 51267 amp Detail 1 Voltage sensor Key Feature e Standard banana plugs and alligator clips The Voltage Sensor provides a simple connection between a ScienceWorkshop interface and an electronic circuit Typical Applications Team CajunSat 9 FRR v3 0 Study resistance voltage and capacitance in circuits e Electroplating Conduct power amplifier experiments Specifications Voltage Range 10 V AC DC Pin Configuration 5 pin DIN plug CBL Compatibility Requires CBL program supplied by TI or Vernier Software Requires PASCO 8 pin DIN plug Cl 6686 to British Telecom Plug Adapter to emulate CBL Voltage Sensor Please call Tech Support at 1 800 772 8700 or 1 916 786 3800 for more information about the adapter Table 11 3 This is the specifications for our volage sensor http store pasco com pascostore showdetl cfm amp DID 9 amp Product_ID 51388 amp Detail 1 Team CajunSat 92 FRR v3 0 Figure 11 3 This is a picture of the voltage sensor http store pasco c
31. 4 in thermal printer and storage pack TDSAF5P Table 11 12 This is a table of the hard copy capability of our oscilloscope http www tek com Measurement cgi bin framed pl Document Measurement Products catalog tds300 specs html amp FrameSet oscilloscopes Team CajunSat 131 FRR v3 0 Mechanical Cooling Method Forced air circulation with no air filter Table 11 13 This is a table of the mechanical information of our oscilloscope http www tek com Measurement cgi bin framed pl Document Measurement Products catalog tds300 specs html amp FrameSet oscilloscopes Environmental and Safety Temperature 10 to 55 C operating 51 C to 71 C non operating Humidity Up to 95 RH at or below 40 C up to 75 RH from 41 C to 55 C operating and non operating Altitude To 15 000 ft 4 570 m operating to 40 000 ft 12 190 m non operating Electromagnetic Meets EN50081 1 VFG 0243 FCC Rules and Regs 47 CFR Part 15 Emissions Subpart B Class A palet UL 3111 1 Listed EN61010 Certified CAN CSA C 22 2 No 1010 1 92 Table 11 14 This is a table of the Environmental and Safety features of our oscilloscope http www tek com Measurement cgi bin framed pl Document Measurement Products catalog tds300 specs html amp FrameSet oscilloscopes Figure 11 13 A Figure 11 13 B This is a picture of our oscilloscope running This is a picture of our oscilloscope runnin
32. 5 rat iier at CTS ar mon gnass ve Senso The grounds of wage andor curent sources mus be at the same roage potentia bale pou hem the Jogger to avoid accurate regnas or damage 49 dhe dagger and cables Figure 11 8 continued This shows the all the data on the HOBO http www onsetcomp com Products Product_Pages pdfs h08 00x Ox pdf Team CajunSat 95 FRR v3 0 External Sensors and Input Cables indoor of H8 or U12 Fay ets pe ah ee uei Split core AC current sensors MUN MEME TIE IR D Temperature sensors of full scale w U12 Response time from 10 to 90 of amplitude CTV A approximately 440 milliseconds CTV B approximately 200 milliseconds Air Water Soil temperature sensors Range 40 to 50 C 40 to 122 F in water or soil 40 to 100 C 40 to 212 in air CTV C approximately 100 milliseconds Accuracy w H8 0 5 at 20 C 0 9 at 68 F CTV D approximately 450 milliseconds w U12 0 25 at 20 C 0 45 at 68 F TMCx HD CTV E approximately 490 milliseconds Resolution w H8 0 41 at 20 C 0 7 at 68 F T din ee w U12 0 03 at 20 C 0 05 at 68 F mcs Input current AC current sine wave single phase Response time in air moving 1 m sec 2 2 mph 50 Hz or 60 Hz load power factor 0 5 to 1 0 lead or lag 3 min typical to 90 in stirred water 1 min typical to 90 Voltage rating 600 VAC Sensor diameter 0 5
33. 7 al 70 F see pint a Resolution 04 af 21 C 0 7 at 70 F Response time In sel 15 min typical to W0 wh sensor Inside case 1 min with sensor outsite case Relative humidity userreplaceable RH senso Range 25 tp 95 RH at B F tor Intervals of gt 10 seconds non condensing and non fogging Accuracy Sie see plot b Sensor operating envbonment 5 to 50 C 41 to 122 F non condensing and nan sogging varies Tom 300 15 900 footcandies Light wavelength response see plc c External Input accepts the folowing sensors Temperature sensors TMCa Hr series Splli core CTS for AC current 5 Models from Telare 7001 TEL 7001 and mA ad atte Garam od 0 25 V DC cable CABLE 2 5 8 External 2 5 volt specfications all HB models except d channel extemar 2 5 mm jack extemal Input ground input switched 2 5 V output external input ground connection Is not the same as PC Interface connection ground and should not be connected to any extemal ground HB Channel Externa modeis 2 5 mm Jack ground Input switched 2 5 vols output ground connection uses the same as PC Imerfare connector gound Input range 0 to 42 5 DC Volts Accuracy 10 mV 3 of reading Resolution 10 mV EH Culput power 42 5 DC at 2 mA atthe only during measurements Safe versions cam OU De used wit asse pur devices amy ab nar mama
34. 76 123 19 22311771 19 22914773 59 96 114 17 75712001 60 02 129 20 07349629 20 07976577 60 05 118 18 35262955 59 88 129 20 12042831 20 12672714 60 22 133 20 62719587 59 95 132 20 56430548 20 57073575 60 18 114 17 69220532 59 78 128 19 99785254 20 00412348 61 03 121 18 51702885 59 95 135 21 03167605 21 03825247 59 77 133 20 78249515 60 17 140 21 73088067 21 73765087 60 11 112 17 40205743 60 04 127 19 75569625 19 76186442 60 12 119 18 48661055 60 15 134 20 80647311 20 81295747 59 74 119 18 60420198 59 81 127 19 83166699 19 8378827 60 25 129 19 99686717 60 13 143 22 2113081 22 21823258 59 77 135 21 09501388 60 3 121 18 74119852 18 7470247 60 09 143 17 56327665 60 06 109 16 95003006 16 95532048 59 56 120 18 81723721 60 17 126 19 5577926 19 56388578 59 82 115 17 95480672 60 120 18 67924414 18 6850801 60 18 142 22 03765926 59 82 143 22 32641184 22 33340828 62 2 143 21 47212148 60 3 122 18 89608445 18 90195878 59 97 109 16 97546783 16 98077413 Average counts 128 Flux 19 6 counts Flux 128 counts 6 88 cm x 1 0 000312 min cm min 0 608 counts cm min flux w dead time 22 31102311 18 89749932 20 043021 17 80425555 17 76267158 18 35835869 20 63361688 17 69771636 18 52271646 20 78901323 17 4074844 18 4923748 18 6100398 20 00308887 21 10162997 17 56875573 18 82315974 17 96043323 22 04452389 21 47859267 Comparing the flux we can conclude that the K2645 is getting the same amount of radi
35. 8 5 0 Payload Development suco me eise lupi 47 5 0 Payload Construction oque passt Aere oak iis tek eet li donee unda bd d o tad 54 6 1 Hardware Fabrication and 5 55 6 2 Integration IAIN act dedo etr aset ee aad eiu 56 6 3 Software Implementation and Verification 59 6 4 Flieht Certification Testigos den ird exi eoe a OE eee a Seded 85 T Mission Operations Saito eo o bp b apa boda eee Ronda eme supe teria 67 Tal Teac Reduit Ge nte oet eon atu cid eure coh iode 68 7 2 Flight Requirements and Operations 68 7 3 Data Acquisition and Analysis Plan 68 8 0 Project Mandagemiefit eai eee Paral abi ee i adu Edad o iR P ad a a a d oc aga 69 8 1 Organization and Responsibilities 70 8 2 Configuration Management ascetur 71 S Interface Control oe iret A ge 71 8 3 I Blectrical Mate 71 8 3 2 Mechanical Inter face cse ensuite Terbi m Ea Re e i DAR S qa poe Ue ess 72 8 5 3 Software Interface 72 Bo Gene mak terface sio oa oe https tt ed eite atas 12 Team CajunSat iv FRR v3 0 9 0 Master Schedule etae eere ee ret Met EEN he 73 9 1 Work Breakdown structure
36. Absolute volts DELTA volts time and frequency Table 11 8 This is a table of the cursors of our oscilloscope http www tek com Measurement cgi bin framed pl Document Measurement Products catalog tds300 specs html amp FrameSet oscilloscopes Physical Characteristics Portable Rackmount Dimensions mm in mm in Width w handle 362 14 3 483 19 Height w pouch 191 7 5 w o pouch 165 6 5 178 7 Depth stand 472 18 6 472 18 6 alone w front cover 490 119 3 w handle s 564 222 518 20 4 Weight kg Ibs kg Ibs TDS 300 6 9 15 5 Domestic 13 1 29 14 4 555 Shipping Weight of conversion kit only Table 11 6 This is a table of the physics characteristics of our oscilloscope Waveform Processing Arithmetic Operators Add subtract multiply Single button automatic setup on selected input signal for Anto Serup vertical horizontal and trigger systems A mixed radix FFT routine is applied to the time domain waveforms to analyze frequency content A Hanning Window is always applied to the acquired signal The display uses dBVRMS vertical scaling Table 11 9 This is a table of the wave processing of our oscilloscope http www tek com Measurement cgi bin framed pl Document Measurement Products catalog tds300 specs html amp FrameSet oscilloscopes Team CajunSat 130 FRR v3 0 Non Volatile Storage Waveforms Two 1000 point reference waveforms Set
37. E 105 Team CajunSat vi FRR v3 0 46 47 48 49 50 51 52 53 54 55 56 Expenditire plans ttbi re tbe b bets Heat cast ad 107 Impact DIGIULOS e bar et pape o od sedat hare p A dra 109 1 vain Na 120 EDD temperature SeHSOL er to Pese ger Ie eee tb eR 121 Voltage Sensor Loss bx ultio ipai 122 HOBO SpecifICatlofis cas bes ances toe ier o a ee ideo eode b Pe d NO Pod i ER d 123 Thermal conductivity of single bOX coi eee tee reete Pere eterne undue dus 126 Batteries sees es ecce ccu ee taste cc E E ee 127 Cold ohambet oe codes ade gust east en teet enia dde qe doe cipe teli tel e ve 127 Vac m chamber TD 128 OSCHTOSCODE rea E AE E E Suey E 0 133 Team CajunSat vii FRR v3 0 LIST OF TABLES l Specifications of Spectra T 390 oia e eet pe 32 2 LND 7232 Geiger Tube General 1 5 34 3 LND 7232 Geiger Tube Window specifications etas dn ERN ro De 34 4 LND 7232 Geiger Tube Electrical specifications ue eec eee iere emi acu 36 5 Dimensions of Geiger Counter Coe eo e test yen ho e ete ss bless Pee ge dea 37 0 Data from K2645 Geiger Counter idis 50 1 Muon Interaction density ui ricette aree pe d
38. KH 0 033uF 250V D1 D4 1N4148 4 134148 1N914 D5 D14 1N4007 10 1N4007 DIODE 1A 1000V BATTERY SNAP9V 1 BATTERY SNAP 9V I TYPE LEADS 150mm GM TUBEGMTUBE 1 GEIGER MULLER TUBE 1 1 CD40106 1 CD40106BE HEX SCHMITT TRIGGER IC2 CD4093 1 CD4093BE 4 X 2 NAND SCHMITT TRIGGER J DBL JUMPER Team CajunSat 49 FRR v3 0 R1 R3 R10 R11 R12 R4 R7 R8 R9 T1 T3 1 14 BT20200 BUSI FU CLIP H2645 MR2 P2645 Table 3 5 RA10M0 RA220K0 RA100K0 RAIMO BC557B LT44 14P BT20200 BUSI FU CLIP H2645 MR2 P2645 RESISTOR 1 4W 10M RESISTOR 1 4W 220K RESISTOR 1 4W 10K RESISTOR 1 4W 100K RESISTOR 1 4W 1M BC557B SI PNP UN 50V 0 2A LT44 IMPEDANCETRANSFO 20KPRIM 1K SEC 14P DIL IC SOCKET 300MIL BOLT M2 X 20mm CYL HEAD SPACER 10mm PLASTIC FUSEHOLDER CLIP MESSING BLANK FOR PCB MANUAL NUT 2mm PCB This is the parts list for the Geiger counter Assembly instructions Mount R1 to R3 10M resistors brown black blue Mount R4 to R7 100K resistors brown black yellow Mount R8 and R9 IM resistors brown black green Mount R10 and R11 200K resistors brown black orange Mount C1 220uF electrolytic capacitor Mina the polarity Mount C2 100nF Sibatit capacitor Mount 1uF MKM capacitor Mount C4 1 capacitor MountC5 to C12 33nF capacitors Mount C14 47nF MKM capacitor 1 OMAN HAN gt 13 Mount C13 which may be eith
39. LaACES Program Flight Readiness Review Document for the Cosmic Ray Experiment by Team CajyunSat Prepared by Team Spokesperson Robert Moore Date Team Member Ross Fontenot Date Team Member Jasmine Bulliard Date Team Member Donald Crouch Date Submitted Reviewed Revised Approved T Gregory Guzik Date John Wefel Date Karen Johnson Date Brad Ellison Date Jim Giammanco Date Team CajunSat i FRR v3 0 Change Information Page Title FRR Document for Cosmic Ray Experiment Date 5 23 2005 List of Affected Pages Page Number Issue Changed some science goals to technical goals 3 23 05 Cosmic ray section added to science goals 3 25 05 Geiger counter section added to science goals 3 25 05 Surface area section added to science goals 3 23 05 Flux section added to science goals and changed flux 3 23 05 formula Muon section added 3 30 05 23 Non vertical section added 4 1 05 23 24 Relativistic effects of muons section added 4 1 05 24 26 Interaction Depth added 4 1 05 27 Slant depth added 4 1 05 30 Second Box design added 3 30 05 31 HOBO was removed from document 4 1 05 32 Interfacing recovery edited 4 1 05 33 Interfacing recovery section fixed 4 1 05 35 Power budget paragraph added 4 1 05 36 Mechanical design fixed 4 1 05 37 Weight Budget error fixed 4 1 05 4 Sample of software code 4 1 05 45 Interface board changed to BalloonSAT 4 1 05 49 Time line error f
40. X FLUX htm 9 FRED CDR document http atic phys lsu edu aces Teams 2002 2003 FLUX FLUX htm 10 HOBO http www onsetcomp com Products Product Pages HOBO H08 H08 family data logg ers html Anchor HOBO 23240 11 http www aboutnuclear org view cgi fC Radiation_and_ Radioactivity Types of Radia tion Team CajunSat 1 3 0 12 Student Ballooning for Aerospace Workforce Development Guzik T G and J P Wefel Louisiana State University August 9 2004 13 Phillips Tony Ballooning for Cosmic Rays http www firstscience com site articles balloon asp 14 University of Leeds What are Cosmic Rays http www ast leeds ac uk haverah cosrays shtml 15 How a Geiger Counter works http nstg nevada edu PAHRUMP handoutcont2 html 16 http polaris phys ualberta ca info Phys29x Manual 11GM01 pdf 17 Muons http www Ibl gov abc cosmic SKliewer Cosmic Rays Muons htm 18 Interaction Depth http www lbl gov abc cosmic SKliewer Cosmic Rays Interaction htm 19 http www answers com topic geiger mueller tube 3 0 Mission Objectives The mission objective of this experiment is to measure the flux of the secondary cosmic rays with respect to altitude 3 1 Science Goals The scientific goal of this experiment is to measure the total cosmic ray flux or rate of flow of radiation per unit area of the cosmic rays in the atmosphere with respect to altitude However this will not be a total flux because we do not expect to detect any alpha par
41. a Particle 49 y y s fy 5 7 15 Beta Particie T 40 Beta Particle Beta Particle Beta Particle Y 4 4 9B ow du 49 Area of our 49 y Geiger counter Y sarace Y Beta Particle 46 fom i A Figure 3 18 This picture shows that the Geiger counter tube will be spinning mostly along the z axis and the radiation will mostly be coming from the top down making the Geiger counter area a rectangle to the particles This is shown by the blue box around the Geiger counter Also alpha particles are not shown even though they are present in the atmosphere they will not be able to get through the two layers of foam core Calculations of Area of the Geiger Muller counter K2645 Dimensions of Geiger counter Length 2 287 cm 0 05 mm Width 0 516 cm 0 05 mm Table 3 6 This is our measurements of the active area of the Geiger Muller tube Area 2 28T7cm x 0 516 cm 1 180092 cm Team CajunSat 31 FRR v3 0 1 E error Ik length x width x Sine de z Jo 2 error p ik 22 87x107 m x 5 16x 10 m x Sine de Jo 2 Average area 0 751 m Every thing in science has error and this experiment is no exception To show the error in our calculations we will use error bars Our error bars are calculated using the average area formula See the following 2 UT 2 E Ta 1 17 x10 Team CajunSat 32 FRR v3 0 4 2 System Desi
42. amber Team CajunSat 98 FRR v3 0 Figure 11 11 This is a picture of our cold chamber 11 3 Vacuum Testing The final single test we will do is a vacuum test of the equipment We must make sure nothing happens to our equipment at a low altitude because all of our equipment we are using is off the shelf and was never intended to be put at an extremely low pressure environment Our tests so far have shown that the equipment we are using can operate in a low pressure environment Figure 11 12 A Figure 11 12 B This shows the inside of our cold chamber with the vacuum A picture of our vacuum chamber chamber inside of it We created a latter like structure to create convection and speed up the cooling process Team CajunSat 99 FRR v3 0 11 4 Test of RF emission To test if our payload was emitting radio frequencies we used a Tektronix TDS 340A oscilloscope To test this all we did was connect our payload to the oscilloscope and measure the frequency We noticed that it did not have any extra frequency at measurement therefore we conclude that it does not emit any radio frequency The following shows our measurements and the technical data on the Tektronix oscilloscope Signal Acquisition System Bandwidth 100 MHz Sample Rate 500 MS s on each channel Channels Two identical channels each with invert function Sensitivity 2 mV to 10 V div with calibrated fine adjust Position Range 5 divisions DC
43. ample rate of 250 000 Hz when using a single channel Features e 250 000 Hz Sampling Rate Sample at 250 000 samples per second on a single analog channel Students will see a true real time oscilloscope and incredibly responsive sound sensor data Built in 1 5 W Function Generator Any experiment requiring a frequency up to 50 KHz and 1 5 watt 300 mA output can be run without additional power amplification Output current and voltage can be monitored internally by the 750 Interface e 20 KHz oscilloscope With the 750 s increased sampling rate the oscilloscope becomes a real time scope with refresh rates up to 40 frames per second e Reduced Noise and More Accurate Data When sampling at rates less than 100 samples per second circuit noise can be visible on a data graph The 750 Interface however provides 8X oversampling to reduce noise and provide smoother data curves e Serial Port Convenience A serial port is available on this SCSI version for an additional connectivity option Unique Characteristics e Ports 4 Digital 3 Analog 1 Output Connection SCSI Serial Data Sampling Simultaneous Analog and Digital Recording e Analog Rates Up to 250 000 samples sec 20 KHz Oscilloscope Team CajunSat 87 FRR v3 0 e Digital Rates 0 1 msec digital timing accuracy 1 mm resolution for Motion Sensor e Function Generator 0 50 KHz 1 5 W 300 mA output Power Amp Compatible e Designed for Advan
44. article s path Reference 17 3 1 3 Non Vertical Muons Muons arriving at some angle 0 from the vertical will have traveled a path length that increases as 1 5 0 See Slant Depth This assumes that the Earth is essentially flat less than 1 error for 0 70 and that muons do not decay over the extended path length Reference 17 Team CajunSat 18 FRR v3 0 If we assume that twice the path length would attenuate the muons to half as many then we would expect the muon flux to vary as the cos 0 However the observed distribution is proportional to cos 0 This is a difference of less than 10 at an angle of 27 and 20 at 43 This difference may be primarily due to the approaching decays of muons as the path length exceeds their range Reference 18 3 1 4 Interaction Depth The energy of charged particles is progressively absorbed by ionizing the matter it passes through The greater the matter and the greater the distance the more absorption Cosmic rays pass through a great variety of environments from the almost absolute emptiness of extragalactic space to the relative mess of our atmosphere to the extreme density of our Earth or even lead shielding We need to measure the path length that would help us predict the absorption At any point along the path the number of interactions is proportional to the density r times the path length dr If we were to add up all of these interactions along the particle s path we wou
45. ation per square centimeter Therefore we can now conclude that our K2645 Geiger counter is ready to be flown Team CajunSat FRR v3 0 6 1 4 Calibration of Geiger counter at sea level To make sure that our flux is accurate we will run our Geiger counter at sea level for a few hours and then compare it to the flux at sea level which happens to be the following 1 0 counts FIUXsea level THEN cm min Once our flux at sea level is correct we can expect our flight to resemble Figure 3 19 This is a theoretical curve for the flux per altitude We notice that we should have an exponential growth until we reach approximately 15 km then we expect it decay exponentially after this point The reason for this has to do with the interaction length of the particles and we be explained in the next section 6 1 5 Calibration of Geiger Counter The Geiger counter we will be using to calibrate the K2645 Geiger counter is a Spectech ST 350 counter made by Spectrum Techniques with a LND 7232 Geiger Muller tube made by LND Inc The specifications on each of them is as follows Team CajunSat 50 FRR v3 0 Spectech ST 350 counter Specifications Input High voltage Display Modes Audio Data Link Power Dimensions Software supplied BNC connector Accepts standard Geiger tubes 0 to 1200 volts digitally selectable in 25 volt increments 6 decade LED 1 in numerals Displays counts preset counts time prese
46. c pressure at sea level is defined as 101 325 Pa The depth X is therefore equal to 10 000 kg m or 1000 g cm As divers know a depth of 10 meters in water density 1 g cm provides an additional atmosphere of pressure In other words 10 meters of water will provide the same absorption as the entire thickness of the atmosphere Reference 18 Team CajunSat 20 FRR v3 0 Interstellar Space Material Air at 15 000 m muon production zone Air at 12 500 m max KAO experiment Air at 4 000 m Top of Mauna Kea Sea Level Air Water Rock Iron Lead Table 3 1 Density g cm 10 0 00019 0 00029 0 00082 0 00125 1 5 8 11 Thickness 1 Atm Equivalent 100 million LY 53 000 m 34 000 m 12 000 m 8 000 m 10m 2m 1 3m 0 9m This chart shows different materials with their densities and their equivalent to 1 atmospheric pressure http www lbl gov abc cosmic SKliewer Cosmic_Rays Interaction htm Altitude ft m 233 000 71 000 105 000 32 000 49 000 15 000 41 000 12 500 36 000 11 000 13 000 4 000 0 0 Table 3 2 Note Top of Std Atmosphere Halfway Zone of Muon production Max alt KAO experiment Top of Mauna Kea Sea Level Density g cm 6x10 1x10 2x10 3x10 4x10 8x10 1x10 This chart shows different altitudes with their density pressure and depth http www lbl gov abc cosmic SKliewer Cosmic Rays Interaction htm Team CajunSat 21 Pre
47. ce between CajunSat team members e Interpersonal communication will occur at CajunSat team meetings to provide weekly updates on progress Email telephone and face to face communication will be used to convey important messages between team members Interface with Stakeholders e Interfacing between CajunSat team members and Stakeholders will be in the form of written PDR CDR and FRR Formal presentations will also be prepared and will allow direct interaction Interface with Project Management e Interfacing between CajunSat team members and project management will occur via interpersonal communication either during scheduled team meetings and office meetings 9 0 Master Schedule The following two sections are the overall work flow plan Any changes to these will follow procedures listed in section 8 2 The tasks listed in the WBS were assigned to the various team members according to their strengths Any team member who is not assigned a task for a specific date will assist others with their tasks All dates listed are on our scheduled work days Thursday and Friday If for some reason we can not finish any particular task on the scheduled date it will be accomplished during the rest of the week There are many times during Monday through Wednesday where we have free time to meet This will aid in finishing all tasks in the manner and timing set forth in the Gant chart Any additional time needed will push the final few tasks into early May
48. ced Placement and College Physics Team CajunSat 88 FRR v3 0 Specifications Power SCSI Computer Connection Serial Computer Connection Digital Channels Analog Input Channels Electrostatic Discharge ESD protected 12 Bit Analog to Digital Conversion Analog Output 12 VDC to 20 VDC at 2 A 2 1 mm jack 8 bit width MDB50 female internal active termination Serial RS 232 8 pin MDIN female 19 2K bits s 1 8 1 4 identical channels TTL compatible 8 mA max drive current Maximum input logic transition time 500 ns Edge sensitive sampled at 10 KHz 1 us res for Motion Sensor 3 identical channels with differential inputs and 1 MOhm impedance 10 V maximum usable input voltage range 12 V absolute input voltage range 3 voltage gain settings on each analog channel 1 10 and 100 Small signal bandwidth up to the ADC 1 MHz for a gain of 1 800 KHz for a gain of 10 and 120 KHz for a gain of 100 input amplifier slew rate 1 2 V us Both digital and analog inputs have ESD protection 5 inputs channels A C analog output voltage and current Voltage resolution at ADC input 4 88 mV 488 mV at a gain 0 049 mV at a gain of 100 Current measurement resolution 244 1 V 50mA mA Offset voltage accuracy lt 3 mV For measuring full scale the total error is less than 15 mV accounting for the gain err input amplifier Sample rate range once every 3 600 seconds 250 KHz Con time for consecutiv
49. composite video Triggers on broadcast standard Trigger Formats NTSC PAL or SECAM video and other interlaced and noninterlaced and Field Rates video with horizontal line rates from 15 to 65 kHz in 5 ranges and field rates from 50 to 60 Hz Table 11 6 This is a table of the trigger system of our oscilloscope http www tek com Measurement cgi bin framed pl Document Measurement Products catalog tds300 specs html amp FrameSet oscilloscopes Display Sin x x Interpolation Vector Connects sample points to display a continuous waveform Dots Displays sample points only Vector Accumulate Mode Accumulates waveform points over a pre set period of time 500 ms to infinity and superimposes the current waveform with bright vectors Accumulates waveform points over a pre set Dou socumulate Mode period of time 500 ms to infinity Format YT and XY Table 11 7 This is a table of the Display of our oscilloscope http www tek com Measurement cgi bin framed pl Document Measurement Products catalog tds300 specs html amp FrameSet oscilloscopes Period Frequency Width Width Rise Time Fall Time Duty Cycle Team CajunSat Automatic Measurements Duty Cycle Amplitude Overshoot Mean Overshoot Cycle Mean High RMS Low Cycle RMS Max Burst Width Min Pk Pk 101 FRR v3 0 Cursors Types Horizontal bars vertical bars paired volts time Measurements
50. e 11 17 Table of what can go wrong and our reactions Team CajunSat 135 FRR v3 0 Problem Solution All electrical components fail Rewire everything so that it works Unable to activate electronics at launch date Make sure everything is connected properly put fresh batteries inside and do everything we can to make it work before flight Hardware failure in flight Decipher what data we have figure out what went wrong and fix the problem so it won t happen on the next flight Software failure in flight Decipher what data we have figure out what went wrong and fix the problem so it won t happen on the next flight Resistors fail in flight Learn why they failed and fix that problem for next flight Temperature drops to below operating range Try to retrieve our data and make sure we have lots of insulation to make sure it can survive without heaters Another team s experiment interferes with our measurements Run some tests and find out the amount of interference and then subtract it from our data Impact destroys payload Retrieve what data we can Data does not match model Find out the source of the error and subtract it from results Run out of human resources Recruit more people and work longer hours Payload weighs too much Get rid of the excess weight Run out of money Find more money from other sources Table 11 18 Everyt
51. e channels in a burst is 2 9 us 8X oversampling for better accuracy at sample rates less than to 100 Hz DC value ranges 4 9976 V to 5 0000 V in steps of 2 44 mV Accuracy at the DIN connector 3 6 mV 0 1 full scale Peak to peak amplitude adjustment ranges for AC waveform 0 V to 5 V in steps of 2 44 mV AC waveform frequency ranges 0 001 Hz 50 KHz 0 01 Maximum amplified output at the banana jacks about 300 mA at 5 V current limited at 300 mA 12 mA Table 11 1 This is the specifications for the Cl 6450 Scientific Workshop http store pasco com pascostore showdetl cfm amp DID 9 amp Product_ID 1487 amp Detail 1 Team CajunSat 89 FRR v3 0 Fr 5 z jh ih IL I C 5 Figure 11 0 This is a picture of the Cl 6450 Scientific Workshop http store pasco com pascostore showdetl cfm amp DID 9 amp Product_ID 1487 amp Detail 1 RTD Temperature Sensor Key Feature e Large temperature range PASCO s resistance temperature device is a highly accurate Temperature Sensor made from platinum wire Comes with a Teflon cover for use in harsh liquids or chemical solutions Typical Applications Conduct experiments where temperature to within 0 5 C is required Measure temperatures down to 200 liquid nitrogen Specifications Temperature Range Accuracy Resolution Output Voltage Temperature ratio Temperature Sensing Junction Pin Configuration 2
52. elleman INC There were no English versions available BEE IBS J m OS seen Figure 3 16 Schematic drawing for the Geiger Muller Counter K2645 from product manual Team CajunSat 51 FRR v3 0 ca Ic Vv F NI NG ICI 7 10 IC2 VELLEMAN K2645 GEIGER MULLER COUNTER Figure 3 17 Schematic drawing for the Geiger Muller Counter K2645 from product manual The following is the method that we will use in constructing our payload however while we are doing this we will also be adding everything to the PDR CDR and FRR This is not stated in the procedures but it will be done 15 2 Build and test a cold chamber to house our payload vacuum chamber and dry ice with the ability to maintain a temperature of about 60 C Do a vacuum test of all the components of our payload to see if it out gases and can function in a low pressure environment Cold test all of the components individually to find the minimum operating range of the components and the max lower temperature possible for it to still function Design and test our box for both structural and thermal support Complete the BalloonSAT and Geiger counter Complete and Test the software to run the BalloonSAT and Geiger counter Complete and test the heating circuit Integrate the heating circuit to the BalloonSAT Find the Dead time for the payload Complete full systems test of t
53. ensity increasing with altitude Right Hess s balloon http www ast leeds ac uk haverah cosrays shtml Cosmic ray composition Cosmic rays are made out of all the particles in the periodic table and are approximately the following portion 89 hydrogen protons 10 helium and 1 of the heavier elements such as carbon oxygen magnesium silicon and iron Reference 1 By studying cosmic rays we can know what the composition source of the cosmic rays Also Cosmic rays are the few examples of matter from outside of our solar system and by studying them we are able to understand how our galaxy evolved the reason for the matter in our universe and our origin Reference 3 High energy cosmic rays When the high energy cosmic rays collide with the atoms in Earth s atmosphere they produce a shower of secondary particles See figure 3 5 The amount of particles reaching Earth s surface is related to the energy of the cosmic rays The frequency of the energies also changes Cosmic rays with energies of greater than 10 eV is about 100 per m and once per century for energies of beyond 10 eV It is these secondary particles that reach Earth s atmosphere with an average flux of about 1 per m per minute For our experiment we will use a Geiger counter to measure the secondary cosmic rays Reference 14 Team CajunSat 5 FRR v3 0 Fluxes of Cosmic Rays 1 particle per m second Flux m sr s Knee 1 particle per m vyeor
54. er one big capacitor of 33nF 1000V or two capacitors of 47nF A400V in series Mount D1 to D4 smaller signal diodes 1N914 or 1N4146 Mind the polarity Model 1n4148 may be color coded wide yellow band brown yellow grey In this case the wide yellow band should correspond to the mark on the printed circuit board If the diode shows number only the black band should correspond to the mark on the pcb Mount D5 to D14 1N4007 type diodes Mind the Polarity Team CajunSat 50 FRR v3 0 14 15 16 17 18 19 20 21 Mount link J next to IC1 Mount a 14 pin socket for and 2 Mount T1 to T3 BC557 558 or 559 type transistors Solder the black wire of the battery connector to battery to the red wire to Mount the transformer LT44 Mount 40106 type with the recess pointing to Mount 1C2 4093 type with the recess pointing to IC1 Mount G M tube take away the small ribbon if any winded around the tube The clip on the anode pin as to be pulled off very gently from the tube Never solder directly to the tube Solder a short strip of wire 2cm to the anode clip and connect it to point A on the PCB Fit the tube socket on point K and then break off the small tooth at one end of it see figure 3 11 and 3 12 After soldering is done and only then you gently push the anode clip back on the tube and fit the tube carefully in its holder NOTE This came from a translated product manual from V
55. erature gets too cold inside and get inaccurate data with Jasmine Bulliard f Donal h range insulation of box and good insulation graphs of step functions Failure to meet Increase level of Increase level of work Deadlines passing Robert Moore scheduled deadlines work without accomplishments Another team s Talk to other groups Take measurements High count rate that Robert Moore experiment might to see what using to on ground with the is not inline with the give off radiation minimize error Geiger counter and curve or other teams and introduce error then subtract that results much yt Extract any available E sgniireani inpact information from Build iesmone 2 Damaged by impact Robert Moore damage lots of stress testing sensor Try to fi t th Try to attribute the Cd ui Flux curve that does Data does not match reason for this error data to something not match model or Robert Moore model and subtract it from else other team s data results Other obligations Try t t LE Recruit more people leave people not to Robert Moore resources people iliendneebines Take out what we do ai Weight budget is Try to get rid of the notnsedor ODE Weight exceeds 500g Jasmine Billiard exceeded excess materials Donald Crouch on the glue Run out of money Find more funding Find more funds No money left in budget Ross Fontenot Tabl
56. g Team CajunSat 132 FRR v3 0 11 5 Complete system test of all equipment and in all conditions The last test we will do is a full system test of our entire payload We will place our vacuum chamber in our cold chamber and let it run for about five hours After this we will take the payload out of the vacuum chamber and drop if from about 8 feet to make sure it can survive the cold and vacuum environment for 5 hours then the impact This test is currently pending t Detection Cannot calibrate Geiger Muller counter K2645 electrical components fail to work Unable to activate electronics Run out of time Software failure Hardware failure heaters fail Temperature drops to below operating range Flight 1 1 Another teams experiment will 4 Flight interfere with our measurements 1 Post flight Will not find balloon payload Impact destroys everything inside including data Data does not match model Run out of human resources Weight budget is exceeded Money budget is exceeded Table 11 15 This shows the likelihood of what will go wrong 1 Post flight Team CajunSat 133 FRR v3 0 Probability Probability of complete destruction Total damage to V Ver ayload ery i i y pay Likely Likely Probable Unlikely Unlikely e Unable to activate e Electrical electronics components VEHI Hardware fail to work ES m Failure e Software fail Extreme Impact failure e Out of destroys data e Out
57. ger coutter experiment e ore qur iban tabes arie t WEST d ds eode 21 8o 751 320 ovt te 26 TO Cram sensitivity CUEVO a iud uod oed estu ute ua 29 TT LND 7232 leti oi tended vetta to t A dead 29 TALC UR eres 31 13 K2045 Geiger C R a 32 14 Count tat of K2645 uerit ertet Sea edite cue re d e a S bU ERE E t e edd 33 15 Schematic or 7645 pet E RE EON Eu PUE e ER NE PILAE 36 16 Environment for payload Gaucunis cete ete deep De os a tub desees up igen UU coto 37 17 Dead tim xp riment mee M e eu Eb ers 39 PSs Theoretical MUX CUYO eei nars toties va buie ERR A 52 19 op c aii 53 PA argo ordei 5 55 21 Primary cosmic rays The aet lon ua eunte ee o 59 22 FRED s 60 235 Montana University ENE ERER hera PO Mud 60 ZA SOME BOX Cia Dram uct 61 25 Building the o ter DOR iuc 62 25 OUEST DOK PICU SS edu avete OR quld 63 2T Inner box d meri ewan end aen or dese ea
58. gn Data Storage Thermistor Switch BalloonSAT board Geiger eiger Muller Heater Counter Data Storage Fig 4 3 Major Components of payload Heating Circuit Resistors Batteries BalloonSAT Board Geiger Muller counter Switch Batteries Figure 4 4 Interfacing of systems Team CajunSat 33 FRR v3 0 BalloonSAT Computer Balloon Ground Team Figure 4 5 Interfacing of recovery Results Graph There will be electrical interfacing between the following Geiger to BalloonSAT Heaters to BalloonSAT Batteries to BalloonSAT Switch to batteries There will be the following Structural Interfaces Board to payload Geiger to payload Heaters to payload Switch to payload Batteries to payload Payload to Balloon There will be the following software Interfaces Geiger to BalloonSAT BalloonSAT to personal computer Team CajunSat 34 FRR v3 0 4 3 Electrical Design 7 Output to G M tube BalloonSat board Figure 4 6 A Geiger Mueller counter schematics The modification in order to couple with BalloonSAT board is shown VCC From Geiger Counter to U2 U1 BASIC Stamp Microcontroller BS2P24 U2 EEPROM Memory 24LC64 U3 Power regulator Figure 4 6 B Interfacing BASIC Stamp with Geiger Counter Kit Team CajunSat 35 FRR v3 0 Notations correspond to the ones used in BalloonSAT Assembly Manual
59. he flux of each detector we will place a Strontium 90 beta source 9 cm away from the detector We will then record the counts once per minute and then calculate the flux with our measured data After completing this experiment we calculated the fluxes of each Geiger counter to be the following Team CajunSat 57 FRR v3 0 2645 Geiger Counter 44 minute run Minutes Counts Minutes Counts Minutes Counts 15 30 30 37 1 28 16 34 31 35 2 38 17 36 32 26 3 39 18 37 33 34 4 24 19 34 34 44 5 43 20 31 35 37 6 36 21 27 36 31 7 46 22 39 37 31 8 33 23 45 38 33 9 50 24 29 39 41 10 36 25 26 40 30 11 46 26 43 41 31 12 22 27 42 42 25 13 39 28 31 43 33 14 31 29 32 44 18 Average 34 counts Table 3 7 This is the Data from one of our runs with the Geiger counter Flux Flux Team CajunSat 20 0 counts 34 counts min 58 min 1 18 cm x 1 0 00654 min 0 203 counts FRR v3 0 LND 7323 Geiger counter data flux w Time counts flux dead time 60 05 143 22 24089852 22 24784146 Time counts flux 59 87 110 17 15982007 17 16519297 59 88 143 22 30404068 59 7 139 21 74551872 21 75234684 59 82 121 18 89157925 60 06 128 19 90462246 19 91083506 60 13 129 20 03677444 59 9 118 18 39858772 18 4043456 59 82 114 17 79867797 59
60. he payload to make sure we are getting accurate results and can survive assembled together with all the items of our payload Team CajunSat 52 FRR v3 0 Build and test cold camber Complete and test Software Complete and test heating circuit Team CajunSat Vacuum test all components Complete the BalloonSAT and Geiger counter Integrate the heaters with BalloonSAT Full systems test under all conditions 53 Cold test each component Design and test box used for payload Find the Dead time for payload FRR v3 0 6 1 Hardware Fabrication and Testing i i ps TITTTTTITITITITIT TT Tit TITTITITTITITITITILIT TTT TTT tt Table 6 1 i f This shows the flow of our hardware fabrication and testing Team CajunSat 54 FRR v3 0 6 1 2 Dead time Geiger Counter One of the things that must be done is calculating the dead time of each detector because without this information we will get inaccurate data We will find the dead time by performing an experiment created by the Syracuse University Physics department and can be found at the following address http www phy syr edu courses PHY344 05Spring Geiger Mueller counter pdf Team CajunSat FRR v3 0 have 100 measurements Move the shelf and source to the top slot and repeat the measurements in the previous paragraph again for 100 measurements 5 Data analysis 5 1 Source count rates Fro
61. hing that can go wrong and our response to it Data logger device made by the Onset Computer Corporation 12 0 Glossary ACES Aerospace Catalyst Experiences for Students ADC Analog to Digital Converter CDR Critical Design Review EEPROM Electrically erasable programmable read only memory FRR Flight Readiness Review GPS Global Positioning System device HOBO NASA National Aeronautics and Space Administration PDR Preliminary Design Review RF Radio frequency RTD Resistance Temperature Device TBD To be determined TBS To be supplied WBS Work breakdown structure Team CajunSat 136 FRR v3 0
62. his is what happened to our battery section Team CajunSat 85 FRR v3 0 Figure 11 2 L This is a close up of our inner box The holes are where we slide in a section of the Balsa wood or section Figure 11 2 M This is a close up of our inner box The holes are where we slide in a section of the Balsa wood or section Team CajunSat 86 FRR v3 0 11 2 Cold testing Cl 6450 Scientific Workshop The instrument we use for our experiments is Cl 6450 Scientific Workshop 750 with SCSI interface with various probes that attach to it Everything is made by PASCO scientific Key Features SCSI Serial Interface e Designed for Advanced Placement and College Physics e Real time Oscilloscope Capable e Built in Function Generator PASCO s 750 Interface is the measurement center for the modern physics laboratory Using a computer and the 750 Interface students can measure force position temperature pressure angular velocity acceleration current magnetic field and more Each 750 Interface includes a built in function generator and real time oscilloscope mode Seven Input Channels With the 750 all 7 channels may be used simultaneously There are no limitations on what combinations of sensors can be used Analog and digital inputs may be mixed in any combination e Four Digital Channels Use up to 4 Photogates or 2 Rotary Motion Sensors a photogate and Motion Sensor Il or any other combination Three Analog Channels Max s
63. ification Testing Conditions o Temperatures 60 C Low pressures 1 atmosphere Rotation around the z axis Possible turbulence Impact 6 m s O Compensation and Testing o In order to ensure a successful flight we will test all equipment multiple times This includes doing vacuum cold and impact testing both individually and all three at the same time We will do what needs to be done to make sure all of our equipment can survive its environment o All of our testing procedures produce an environment that is a little rougher than what is expected This ensures that our payload will survive and function as it is designed 7 0 Mission Operations The payload will be launched and tracked from the ground by a separate GPS unit It will be recovered upon landing The following operations will be performed pre flight and post flight Pre Flight Operations Full system test of hardware New batteries are to be placed in payload for maximum voltage Check all structures to make sure they are properly fastened down Make sure lids are properly sealed Properly attach payload to balloon Recovery and data extraction Take pictures Record observations Examine for mechanical damages Examine the payload and see if there are any damages in the integrity of the system Disassemble the payload and extract the BASIC Stamp Download the data from EEPROM through the serial cable connection on the BalloonSAT b
64. is is an average of all of our data for each distance 56 FRR v3 0 Volts Run 1 Run 2 800 328 336 775 271 271 750 273 231 725 287 213 700 256 235 675 256 225 650 186 215 625 0 0 Table 3 4 B This is the data for our far distance which was the second slot Counts vs Voltage 1000 _ 900 4 e ec 800 600 _ 500 400 Counts per 60s 300 100 0 v T T T T T 620 645 670 695 720 745 770 795 Volts Figure 3 12 This is our experimental Geiger plateau We can see that the optimal voltage is 725 V Once we figure out the Geiger plateau for the LND 7232 we will use it to make sure that it is operating at the correct operating voltage After this we will take a Strontium 90 source and place it an inch away from the detector We will then take measurements in one minute intervals and calculate the flux After we do this we will compare the results of each Geiger counter Team CajunSat 57 FRR v3 0 in km i 2 6 10 20 Variation of cosmic rays with altitude e a Counting rate coincidences min 800 600 400 200 o Atmospheric pressure in mmHg Figure 6 1 Theoretical calculated flux of cosmic rays with respect to altitude http hyperphysics phy astr gsu edu hbase astro
65. ixed 4 1 05 GAMA SCOUT removed from document 4 1 05 Risk Management errors fixed 4 1 05 Team CajunSat ii FRR v3 0 TBD Section Number Status of TBDs Description Surface area of Geiger Counter tube Date Created 3 11 05 Date Resolved 5 1 05 Gas in Geiger Counter tube 3 11 05 4 27 05 Time interval for the amount of counts 3 11 05 4 27 05 GPS device actually being used during flight 3 8 05 5 2 05 Resistance of heating circuit 3 11 05 4 26 05 Technical Specs of Geiger Muller Counter kit 3 11 05 4 28 05 Will a double box provide better results an a heater 3 31 05 5 3 05 Dead Time 4 1 05 4 29 05 Geiger counter power 4 1 05 4 29 05 BalloonSAT 4 1 05 5 9 05 Team CajunSat iii FRR v3 0 TABLE OF CONTENTS OVES E ua tbt cc teh ees ee hd de Ro ef e of 1 Change Information ea eka LUC otal nun E ii Slats Ol LBD Med iii Table of a EU e PARI Dx UA wa ta Oda V qu HEIC pM NR EAR A iv List ast oie cu duit ure phas Lisbot Fables wont veneta nat ate d gested aa ea ep Ate vi LO Docunient PUrpOSe teer
66. k and the graphs replaced with the double box experiment We are certain that it will work because between the heater and another layer in insulation the box should not get to below our operating of 20 C This is the minimum temperature because after this we get too little voltage which in turn will give us too little current Also our devices are not designed for this low of a temperature so they can become inoperable making our flight a failure To make sure this does not happen we will do lots of testing to minimize the effects of this incase of a heater failure Thermal Conductivity of Double Box Temperature C Time s Time s vs Temperature Oustide C Time s vs Temperature Geiger level internal C Time s vs Temperature Geiger level external probe C Time s vs Temperature BalloonSAT Level Internal temperature C Time s vs Temperature BalloonSAT Level external Probe C Figure 11 9 This shows the thermal conductivity of the box using the HOBO data logger inside it Team CajunSat 97 FRR v3 0 Battery Test Temperature C Voltage V Time s vs Temperature C Time s vs Volts V 500 1000 1500 2000 2500 3000 3500 Time s Figure 11 10 Graph shows that low temperature can make voltage go to zero This means current goes to zero also due to Ohm s Law meaning that none of our devise will work due to lack of power Figure 11 11 A This is a picture of our cold ch
67. ld get a number that should be proportional to the total absorption Reference 18 If density has units of g cm and the path length is in units of cm then this Interaction Depth X has units of g cm At first it seems strange to be talking about some sort of distance with units of g cm but it does allow us to compare the effects of passage through kilometers of the upper atmosphere to passage through a few centimeters of water Reference 18 Figure 3 9 This Picture shows that different angles that the can be formed when the primary cosmic rays reach Earth http www lbl gov abc cosmic SKliewer Cosmic_Rays Interaction htm The pressure here at the surface of the earth although partly due to dynamic effects of air movement is mostly due to the total weight of the air above that point The cross sectional area of a column of air radiating directly upward gets larger as it rises The acceleration of gravity decreases as you get farther away However the earth is so large and the atmosphere so thin that both of these values are essentially constant to within 1 Reference 18 Team CajunSat 19 FRR v3 0 F gdm gpAdr 9 par PA pdr eq II Thus at some altitude h the pressure divided by g 9 8m s is a measure of the absorption along a vertical path to that point The 1967 Standard Atmosphere see article later gives us empirical equations to calculate the pressure at any altitude The standard atmospheri
68. like a bar magnet This also means that it is impossible to tell the exact origin of the cosmic rays Reference 1 Early Research During the 1930 s to 1950 s man made particle accelerators were unable to reach very high energies so cosmic rays served as a source of particles for high energy physics which led to the discovery of the first muon and pion However this is not the only application of comic rays In fact since the beginning of the space age the main focus of cosmic ray research has been towards astrophysical investigations of where cosmic rays originate how they get accelerated to such high velocities what role they play in the dynamics of the Galaxy and what their composition tells us about matter from outside our solar system In order for us to measure cosmic rays directly we must do our research on space craft and high altitude balloons before they have a chance to be broken up and slowed down by Earth s atmosphere Reference 1 Cosmic Ray energies and Acceleration Cosmic rays are usually measured in units of MeV or GeV and their energy range is a little less than 1 MeV to a little over 1 ZeV 10 eV which is about one billion times more powerful than any current particle accelerator See Figure 3 2 Team CajunSat 3 FRR v3 0 Most galactic cosmic rays have an energy range of 100MeV to 10GeV or a velocity range of 46 to 99 5 the speed of light The number of cosmic rays with energies above 1 GeV decreases by a facto
69. lted in a longer wait period that our project could not afford It is possible more money will need to be allocated to purchasing additional supplies batteries heating etc According to the below Fig 10 2 we have 27 of our budget left to cover additional expenses we may encounter 10 1 Expenditure Plan UL Lafayette LaACES Budget 60 00 12 135 00 27 Batteries E Velleman Geiger counter 150 00 Additional supplies for 30 Geiger counter Heating 75 00 15 Building supplies 20 00 50 00 10 00 4 H Testing supplies 10 29 E Left over budget Figure 10 2 This is a pie graph that shows the distribution of funds At this point in time we have purchased batteries the Velleman K2645 Geiger Muller Counter Kit testing supplies and some building supplies The lithium batteries will have two purposes in our LaACES program First we will use at least two batteries for testing voltage drop cold Team CajunSat 77 FRR v3 0 testing vacuum testing and cold vacuum testing The second use for the batteries will be in powering the electrical components within our payload We will use two 9V lithium batteries to power the load Referring to figure 10 2 battery cost was 12 of our budget The Velleman K2645 Geiger Muller Counter was purchased for approximately 150 00 Since it was one of our most costly items 30 of our budget Figure 10 2 we researched multiple suppliers in order to be
70. m the measurements in Section 4 3 determine the measured count rate number of decay particles detected per unit time for each source and for the background Subtract the latter from each of the measured source count rates to determine the background corrected source count rates For each source use the dated source activity the half life and the radioactive decay equation you learned in Physics 216 to determine the source activity number of decays per second today Compare that value to the observed count rate In your report explain the difference in these values Using the 100 s measurement on Co 60 in Section 4 3 calculate the theoretical standard deviation in the observed number of counts Use that value to determine the standard deviation in the count rate for Co 60 calculated above Look at the 1 5 measurements in Section 4 5 with Co 60 source in the top slot Find one of the values that is near the middle of the distribution of observed counts e g one close to the roughly estimated mean value or median value Use that chosen number of counts to calculate the count rate and standard deviation in the count rate Compare these results to those for the 100 s measurement on the same source in the same position Notice that according to theory the standard deviation of the number of counts is equal to the square root of the number of observed counts Thus it increases as the number of counts increases Why then is it better to use a large
71. mic SKliewer Cosmic Rays Interaction htm of the following sections on Muons explained in depth the interaction length of cosmic rays and gave some examples of each 3 2 Technical Goals Our technical goals are as follows 1 Accurately measure the total flux of the cosmic rays with respect top altitude Obtain knowledge of sensors electronics and systems Learn how to develop and maintain a research program Learn how to create different environmental simulation testing Have a successful flight Obtain useful accurate information Dope e Team CajunSat 22 FRR v3 0 The major technical goal of this experiment is to accurately measure the total flux of the cosmic rays with respect to altitude We also expect to get a graph that will look similar to Figure 3 2 To do this we must keep the temperature to no less than 20 C because that is minimal operating range To do this we will be using a heating circuit that should keep the temperature to above 0 C Primary Cosmic Ray nuclaar interaction Em air molecule Xe T ay K Fi V Y Y neige d yx yv Cherenkov amp fluorescence radiation t K H M u H p n T7 Ye TYe nuclear fragments muonic componant hadronic electromagnetic neutrinos component component Figure 3 10 Graph showing the shower of secondary cosmic rays http hyperphysics phy astr gsu edu hbase astro cosmic html 23 FRR v3 0 Team CajunSat c c FRED
72. ns as cosmic rays or particles from a radioactive substance by means of the ionizing effect on an enclosed gas which results in a pulse that is amplified and fed to a device giving a visible or audible indication The exact gas varies for each detector but it always includes a mixture of gases This mixture always includes an inert gas usually neon or argon and organic vapor such as halogen or alcohol vapor Reference 19 The Geiger counter we will be using is the Geiger Muller Counter Nuclear Radiation Detector K2645 This Geiger counter like every other Geiger counter consists of two basic parts the probe and the counter The probe is filled with a gas with a wire down the middle that measures the radiation This probe has two primary functions keeping track of how much radiation is Team CajunSat 26 FRR v3 0 detected by means of a counting circuit and to provide power for every component on the Geiger counter Reference 14 Once power is supplied to the probe a large potential is created making the central wire become the anode and the metal wall becomes the cathode At this stage the gas is neutral until radiation enters the probe creating a shower of particles inside the tube This shower knocks off electrons creating both free electrons and gas ions which force the electrons to be pulled off rapidly to the central wire Once this happens the electrons are collected on the wire are sent through the wire into the counting circuit which
73. number of counts over a large time interval to determine the count rate instead of using a smaller number of counts over a smaller time interval Discuss this point in your report 5 2 Count rate versus distance From vernier caliper measurements calculate the distance from the top of the source to the window of the GM tube for each of the five count measurements in Section 4 4 Convert your count measurements to background corrected count rates at each source position Plot a graph of count rate ordinate versus source to detector distance abscissa Then plot another graph of count rate versus the inverse of the square of the distance If the radiation intensity follows the usual 1 7 relation from an isotropic source and if the Geiger counter measurement is proportional to intensity the latter graph should of course be a straight line through the origin In your report discuss whether or not this is the case and why 5 3 Counting statistics Using the measurements in Section 4 5 with the source in the lower position make a table with three columns 1 the observed values of the number of counts 2 the occurrence of that number of counts i e the number of intervals for which that number of counts was observed and 3 the probability of occurrence of that number of counts Plot your results as probability ordinate versus number of counts Calculate the mean value of the number of counts On the graph of our data plot the appropria
74. oard one at a time Then checks for zero s in all locations of gm eeprom SSTAMP BS2p SPBASIC 2 5 SDgm PIN 8 8 clears G M SCLgm PIN SDgm 1 sdtemp PIN 0 0 clears temps scltemp PIN sdtemp 1 addrlow VAR Word internal address Isb addrhigh VAR Word internal address msb value VAR Byte value to write result VAR Byte array for returned value Write To gm EEPROM value 9600000000 binary zero DEBUG Writing to eeprom 1 CR PAUSE 20 FOR addrhigh 0 TO 255 FOR addrlow 0 TO 255 loop through all addresses I2COUT SDgm A0 addrhigh addrlow value Joad zero PAUSE 10 DEBUG Addr DEC3 addrhigh addrlow Value DEC3 value CR NEXT NEXT PAUSE 20 Write To temp EEPROM DEBUG Writing to eeprom 2 CR PAUSE 20 FOR addrhigh 0 TO 255 FOR addrlow 0 TO 255 loop through all addresses I2COUT sdtemp A0 addrhigh addrlow value Joad zero PAUSE 10 DEBUG Addr DEC3 addrhigh DEC addrlow Value DEC3 value CR NEXT NEXT Read From EEPROM DEBUG CR Reading CR Team CajunSat 63 FRR v3 0 FOR addrhigh 0 255 FOR addrlow 0 TO 255 I2CIN SDgm A1 addrhigh addrlow result DEBUG DEC3 result IF result gt 0 THEN DEBUG error at loc DEC addrhigh DEC addrlow CR ENDIF PAUSE 10 NEXT NEXT PAUSE 100 DEBUG CR locations cleared CR END Team CajunSat 64 FRR v3 0 This program will allow us to get the counts
75. oard and process it on a computer Take a ground test of Geiger counter again to make sure it is functioning properly Data Analysis Check if data has been collected for the entire duration of the flight Plot the flux with respect to altitude using the GPS data from a tracking unit Check if the plotted data agrees with the expected theoretical curve Figure 3 18 Team CajunSat 67 FRR v3 0 7 1 Launch Requirements Final testing check if the separate parts of the payload are operable and are powered on BASIC Stamp Geiger counter heating unit check if the parts interact as designed and work as a whole check power sources for output voltages and currents and replace by a new spare if needed check control points for proper voltages on them check the integrity of the system make sure everything holds firm inside the cube verify GPS synchronization proper sealing of payload and attachment to balloon vehicle All test should give a positive result and all malfunctioning revealed should be taken into consideration and fixed in field A full cycle test run should be done in field This will simulate the data acquisition during the flight This also will allow us to make sure that everything is still functional after the transportation 7 2 Flight Requirements and Operations Flight Requirements payload must reach a height of at least 15 km heating devices must maintain the payloads temperature to a minimum value
76. of time Too heavy money Temperature e Lost drops too low payload Negligible Table 11 16 Risk Matrix e Cannot Calibrate Geiger Counter Interference from other teams experiments Team CajunSat 134 FRR v3 0 Responsible Risk event Response Contingency Plan Trigger Party Try reprogramming Inaccurate readings Cannot calibrate the software or Use the Gamma Scout from a known source Geiger Muller updating a few or another brand of and compared to Robert Moore counter k2645 pieces of equipment or go to back up Geiger counters other Geiger counters available All electronic components fail to work Find some that will work Locate working components Not working Jasmine Bulliard Donald Crouch Software failure in flight Try to decode the data and attempt for possible recovery recover all possible data Unusable data or data that is not synchronized correctly Jasmine Bulliard Donald Crouch Hardware failure in flight Try to find reliable data Recover what we can No data or inaccurate data Jasmine Bulliard Donald Crouch Heaters fail in flight Box is constructed out of insulated materials to help keep heat in Use better or more insulation Temperature inside gets too cold inside Jasmine Billiard Donald Crouch Temperature drops to below operating Resistors failed and must rely on Make sure that we have fresh batteries Temp
77. ol There will be four main interfaces They include 1 Electrical interface Section 4 3 2 Mechanical interface Section 4 5 3 Software interface Section 8 3 4 General interface Section 8 3 Note any changes to the interface design will follow the same procedures listed in Section 8 2 8 3 1 Electric Interface Electric interface is the electronic connection between the subsystems The specific interfaces are 1 Switch to batteries 2 Batteries to BalloonSAT 3 Interface board to Geiger counter 4 BalloonSAT to heaters 8 3 2 Mechanical Interface This is the structural connection between each system The specific interfaces include the following Box to Balloon BalloonSAT to box Heaters to box Geiger Counter to box Batteries to box Switch to box TOU Rm This will following the guidelines in LaACES lecture Payload Construction Considerations and Techniques Team CajunSat 71 FRR v3 0 8 3 3 Software Interfaces The software programming needed to central subsystems store measurements and retrieve data after flight is known as software interfaces It will include the following XU ud Program to provide timing for data collection Program to save raw data Program to convert raw data to formatted data Program to retrieve data 8 3 4 General Interfaces These are the interfaces between the various levels of entire project The specific interfaces are in the following list 1 Interfa
78. om pascostore showdetl cfm amp DID 9 amp Product_ID 51388 amp Detail 1 HOBO A HOBO device is used for us to take the temperature inside our box for testing and for calibration of the thermistors on the BalloonSAT They will not be on our flight The following is the specifications of the HOBO Team CajunSat 93 FRR v3 0 7 Modet Choose Fram 8ir4Br20cm 41902 approximately 29 gm 1 og Measurement Ranges Temperature 20 to 70 C 4 10 158 F FH 255 to 05 at 25 C tor intervals 210 seconds Light Intensity 2 to 800 footcandles lumens tygical light sensor response range mpprax 480 to 800 SS EN 555 over the range of 5 to 50 C 41 to 122 F Operating Range 20 to 70 C 4 to 158 F 0 to 95 relative humidity non condensing non logging FH sensor operating range is 3 30 C 41 to 122 F Figure 11 8 This shows the all the data on the HOBO T HOBO H8 family of data loggers provides easy to use data collection at affordable prices Choose single two or four channel models to measure temperature relative humidity light intensity or external channels accepting external temperature AC current sensors CO input and 4 20mA or DC voltage cables for input from third party sensors Features Easy to Use User celectabie samping intervals 0 5 seconds 10 8 hours reocrdng times up to 1 year Prcgrammabe siart timegata Memo
79. ons http www th physik uni frankfurt de drescher CASSIM red neutrons blue electrons positrons orange protons gray mesons green muons Team CajunSat 9 FRR v3 0 Pouresoc blue electrons positrons This is a computer simulation of the primary cosmic rays interacting with the atmosphere cyan photons http www th physik uni frankfurt de drescher CASSIM red neutrons orange protons gray mesons green muons Team CajunSat 10 FRR v3 0 Figure 3 5 D blue electrons positrons This is a computer simulation of the primary cosmic rays interacting cyan photons with the atmosphere ae red neutrons http www th physik uni frankfurt de drescher CASSIM orange protons gray mesons green muons Team CajunSat 11 FRR v3 0 Figure 3 5 E A blue electrons positrons This is a computer simulation of the primary cosmic rays interacting with the atmosphere cyan photons http www th physik uni frankfurt de drescher CASSIM red neutrons orange protons gray mesons green muons Team CajunSat 12 FRR v3 0 Figure 3 5 F M blue electrons positrons This is a computer simulation of the primary cosmic rays interacting db with the atmosphere cyan p otons http www th physik uni frankfurt de drescher CASSIM red neutrons orange protons gray mesons green muons Team CajunSat 13 FRR v3 0 blue electrons positrons cyan photons red neutrons Figure
80. ormed in the near future for determination of best mounting method for devices inside payload The interfacing of interior parts of the payload can be examined in Figure 4 4a and 4 4b The payload box will be a 15 cm by 15 cm by 15 cm cube box made out of foam board and possibly a second foam board 13 cm by 13 cm by 13 cm This will be so that we can not have to use a heater eliminating weight The components will be properly sealed and cushioned in order to withstand the unpredictable flight and landing The landing could be rough but all we need to recover out of the payload is the memory chip off of the BASIC Stamp Our weight budget was 450 g The battery we are using for all devices is a 9V Lithium Ultra life Longest life battery The specifications on it are as follows Team CajunSat 40 FRR v3 0 ULTRALIFE ETITI ae B INC Li MnOz Primary System U9VL J 9V Size Battery System Lithium Manganese Dioxide Designation NEDA 1604 LC Nominal Voltage 9 0 Volts Capacity C 1 200 mAh 900 Q to 5 4V 23 C Max Discharge 120 mA Continuous Weight 36 4 grams Oper Temp Range 20 to 60 Storage Temp Range 40 to 60 C Z 49 0 1 93 130 051 Volume 226 cm 26 5 17 5 Terminals Miniature Snap 1 04 0 69 Housing Aluminum Mylar Label Dimensions in mm Battery Life Comparison 3000 27 mA Continuous Discharge to 7 2 Volts Wireless Microphone Telemetry Transmitter Test ULTRALIFE LITHIUM
81. r of 50 for every factor of 10 increase in energy The highest energy rays measured to date is 10 eV Reference 1 It is believed that most galactic cosmic rays derive their energy from supernova explosions which occur approximately once every 50 years in our galaxy For cosmic rays to maintain their intensity over millions of years requires only a few percent of the 10 J released by the typical supernova explosion There is also evidence that cosmic rays are accelerated as the shock waves from these explosions traveling through interstellar gas The energy contributed to the Galaxy by comic rays is about that contained in galactic magnetic fields and in the thermal energy of the gas that passes through the space between the stars This is approximately 1 eV per cm Reference 1 While we might be able to detect cosmic ray energies we do not always know how they are accelerated to such a high velocity In fact the source of energy greater than 10 eV is unknown It is believed that they might originate from outside our galaxy from active galactic nuclei quasars or gamma ray bursts but it can also be some exotic new physics such as superstrings exotic dark matter strongly interacting neutrinos or topological defects in the very structure in the universe Reference 3 To better see this see figures 3 2 and 3 3 Team CajunSat 4 FRR v3 0 Figure 3 2 Left Victor Hess before his balloon flight during which he observed cosmic ray int
82. re is not maintained at this level then collected data can become inaccurate and not sensible We are going to use two simple heating circuits figure 4 7a and 4 7b to maintain temperature at operating level The only temperature dependencies will be remaining in operating temperature range in order to collect valid data Team CajunSat 37 FRR v3 0 Thermal Conductivity of Double Box Temperature C 0 1000 2000 3000 Time s Time s vs Temperature Oustide C Time s vs Temperature Geiger level internal C Time s vs Temperature Geiger level external probe C Time s vs Temperature BalloonSAT Level Internal temperature C Time s vs Temperature BalloonSAT Level external Probe C Figure 4 8 This is the results of our heater test 4 5 Mechanical Design Figure 4 8A Figure 4 8A Figure 4 8B Fig 4 8 C Top level second level third level bottom level mmm E Team CajunSat 38 FRR v3 0 Figure 4 2 A Robert Moore building the outside box Mask is used because of the fumes of the epoxy Figure 4 2 B Picture of the outer box Team CajunSat 39 FRR v3 0 Figure 4 2C This is a picture of the inner box See figures 4 1 and 4 3 for a complete picture of the payload It will contain on the bottom the Geiger counter and BalloonSAT figure 4 10a there will be a heating unit On the front face three 9 V batteries will be mounted figure 4 10d Multiple stress test will be perf
83. rmine the appropriate operating voltage The exact procedures used to obtain the graph in Figure 3 8 was designed by the University of Louisiana at Lafayette physics department for the Modern Lab We will not be able to find the Geiger plateau for the K2645 Geiger counter Therefore the plateau will only be used to ensure that our calibration detector is operating correctly Once we have determined this we will measure the flux of both Geiger counters with the same source from the same distance and compare the results After doing this we will find the dead time of each Geiger counter Once we find the dead time we will compare the flux of each Geiger counter The dead time procedures will be explained in a later section After we complete all of this we will know that the K2645 is operating correctly Team CajunSat 27 3 0 To Co axial Detector Cable Probe Housing Probe Gas Cathode Window Gas Atom Electron Q 2 1 1 Gas Figure 4 3 This shows how exactly a Geiger counter works http nstg nevada edu PAHRUMP Microsoft 20PowerPoint 20 20Geiger 20Counter 20Diagrams pdf Team CajunSat 28 FRR v3 0 discharge region Geiger plateau breakdown voltage threshold ounting rate I V Applied voltage Figure 3 7 This is the theoretical Geiger counter voltage curve http polaris phys ualberta ca info Phys29x Manual 11GM01 pdf Team
84. roblem because the batteries are on the bottom and only would break the heaters Figure 11 1 A Figure 11 1 B This is at the bottom of where we roll our foam box This is at the top of where we roll our foam box down down the stairs and then observe what happens the stairs and then observe what happens Team CajunSat 79 FRR v3 0 Figure 11 1 C Figure 11 1 D Figure 11 1 E Pretesting of box Outside of box after we threw it down the What happened on the inside The glue did not stairs hold well and we actually ripped a battery bottom off on upper left picture Figure 11 2 A Picture from the second story window Team CajunSat 80 FRR v3 0 Figure 11 2 B Picture of the second story window where we threw out the box Picture of the landing Team CajunSat 81 FRR v3 0 dx Figure 11 2 D Close up of our box after the landing Figure 11 2 E Close up of our box after the landing Team CajunSat 82 FRR v3 0 Figure 11 2 F This is a picture of the top layer of our payload This is wh aT at will house the Geiger counter vR 4h P Figure 11 2 G This is a picture of the top layer of our payload This is what will house the BalloonSAT Team CajunSat 83 FRR v3 0 Figure 11 2 H This is what happened to our battery section Figure 11 2 I This is what happened to our battery section Team CajunSat 84 FRR v3 0 Figure 11 2 J This is what happened to our battery section Figure 11 2 K T
85. ry modes Step when ful Wrap around when ful Read cut and relaunch with optional HOBO Shute Precision componems eliminate need tor user calbration Mounting kt included magnet anc tape Versatile Seven models trem which to chocse with 1 4 channels to measure temperature humidity ight and extemal inputs Mocek wih extemal input accept extemal sensors for temperature AC current cardon dioxide COs 4 20 mA and 0 2 5 Vors DC intemal temperature sensor on 10 2 wre can extend from case Pelsbie Capacity 7643 measurements total except 4 Chanrel Extemal which stores 32 520 measurements Blinking LEO confirms operation Battery level Indication at launch Nomvolaiie EEPROM memory retains data even 1 baftary tals Time accuracy 1 minute per week at 20 C 65 F NIST traceadie temperature accuracy cemification available Compliance certificate avalabie irtrinsicaity eate extemal avaliable User eolaoeeble lasts 1 year typical Orop proot to 1 5m 5 Bz Car ccezaltie By Boo Cartero cormpatbie Cong lar rsevart Grecives in European Union EJ HCEO conpassie IS rezcaty care http www onsetcomp com Products Product_Pages pdfs h08 00x Ox pdf Team CajunSat 94 FRR v3 0 Time Accuracy 1 minufie week at 20 C 68 F Temperature intemal sensor Range 20 to TOC 4 10 158 F Accuracy 20 7 21 C 1 2
86. s is a picture of our equipment together LND 7232 Geiger Muller Tube General Specifications Gas Filling Ne Halogen Cathode Material 446 Stainless Steel Maximum Length inch mm 4 85 123 1 Effective Length inch mm 2 6 66 04 Maximum Diameter inch mm 1 38 34 9 Effective Diameter inch mm 1 13 28 6 Connector BNC Operating Temperature Range Ko 55 to 75 Table 3 2 This is the general specifications of the Geiger Muller tube http www lndinc com gm alpha 7232 htm Team CajunSat 52 FRR v3 0 Window Specifications Areal Density mg cm Effective Diameter inch mm Material Table 3 3 This is the window specifications of the Geiger tube http www Indinc com gm alpha 7232 htm Electrical Specifications Recommended Anode Resistor meg ohm Maximum Starting Voltage volts Recommended Operating Voltage volts Operating Voltage Range volts Maximum Plateau Slope 100 volts Minimum Dead Time micro sec Gamma Sensitivity Co cps mR hr Maximum Background Shielded 50mmPb cpm Tube Capacitance pf Weight grams Table 3 3 This is the electrical specifications of the Geiger tube http www Indinc com gm alpha 7232 htm Team CajunSat 53 2 0 1 13 28 6 Mica 1 800 900 850 1000 10 150 40 50 3 155 FRR v3 0 4 85 113 CONNECTOR BNC WINDOW Figure 6 10 Circuit drawing for the Geiger tube http www Indinc com gm alpha 7232 htm mGy Hr 10 10
87. se off some of the outer electrons however muons only interact by ionization Because of this muons are able to travel large distances and reach the Earth s surface Their only energy lost is proportional to the amount of matter they pass which is proportional to the density g cm times the path length cm This interaction length has units of grams per square centimeter see Interaction Depth Reference 17 Team CajunSat 17 FRR v3 0 Figure 3 7 This graph just shows the primary cosmic rays entering Earth s atmosphere and creating muons http www lbl gov abc cosmic SKliewer Cosmic Rays Muons htm The Muon energy lost is a constant rate of about 2 MeV per g cm Since the vertical depth of the atmosphere is about 1000 g cm muons will lose about 2 GeV to ionization before reaching the ground The mean energy of muons at sea level is still 4 GeV Therefore the average energy at creation is approximately about 6 GeV Reference 17 The atmosphere is so weak at higher altitudes that even at 15 km it is still only 175 g cm deep Typically it is about here that most muons are generated and also the peak of the flux of the cosmic rays The average muon flux at sea level is 1 muon per square centimeter per minute This is about half of the typical total natural radiation background Reference 17 Muons and other particles are generated within a cone shaped shower with all particles staying within about 1 degree of the primary p
88. ssure Depth Pa 67 868 12 000 18 000 23 000 62 000 101 000 g cm 0 7 9 130 180 230 630 1 000 FRR v3 0 3 1 5 Slant Depth All of the above Depth calculations are true only for muons arriving vertically By simple trigonometry it can be seen that dr distance along the slanted path is equal to dr cos 8 where 0 is the angle of the path measured from vertical Reference 18 Given a slant depth we can use the standard atmosphere pressure equation to extrapolate an equivalent altitude that would correspond with this depth if it were vertical This will allow us using ground level measurements to extrapolate the muon intensity vs altitude graph from the KAO experiment to negative altitudes i e below sea level Reference 18 In the following table X X cos 0 The Equivalent Altitude uses the 1 layer pressure equation from the standard atmosphere model The last three columns are provided as a comparison to the observed cos distribution to which the particle data book refers The discrepancy is most likely due to muon decays Reference 18 0 Slant Depth X Equiv Altitude Xo cos 0 0 cos g cm m g cm 0 1 034 0 1 034 1 1 15 11 070 293 1 108 0 966 0 933 30 1 194 1230 1 378 0 866 0 750 45 1 462 3 022 2 068 0 707 0 500 60 2 068 6 249 4 135 0 500 0 250 75 3 994 13 000 15 432 0 259 0 067 Table 3 3 This graph shows the various angles http www Ibl gov abc cos
89. t aie Rese ease 65 2S 66 29 Taner od cue Res DEO EI ER oL 67 30 Inner box SECTIONS sie trice eid aeq in tard aie raura 68 o1 Inher box SUDDOLE e ar p d Re apa este utis ids 70 32 Systemi de TOTIS slap tet ne atu boue ce cede ete 19 233 Interfac mp Of SY SPE TING o oe e Roe py abe de ed ddp ad s ns 74 34 Interfacing OF TECOVELY electa be und nda east Nd Rd 74 35 Geiger Muller ua a oce de bein cac decia e rie apis Ebo doles 75 DO Circuit desioen a eto aun ct tesa ds wa nace d ou de 77 dato Sb basalt ted tah citet Sel TI 38 Ultra life A a edet adu aiias 79 39 VIC O3 I TL 81 40 Calibration oeste b SER E I NN M LH NM Ln M e oe ot 81 41 Weicht UC tras uS e ce A bem asume 87 BD Wis POP CAC UE NIRE 88 43 Flow of constr ction eee qr ete tercie etre eee eter ee dase d ea 92 447 SOW WATS arcus estela ce it tet ai Sian ease Ide iti Pup es 95 AS Eme lifleo ausa oci endete MD E
90. t time CPS alarm level and high voltage Count for preset time count for preset count counts min counts sec set alarm level 0 999999 cps set high voltage 0 1200v and remote Piezo alerter if countrate exceeds preset level DB 9 male connector accepts RS 232 serial cable Input 7 5 volt DC at 500mA from AC line charger Specify 110 120 220 240 VAC at time of order Battery option requires installation of 4 x C size NiCd rechargeable batteries not supplied 12 in W x 8 in H x 4 5 in D ST350 Radiation Counter PC emulation software DOS program runs on most IBM compatible PC s including CGA EGA VGA SVGA and Hercules graphics systems Real time display of simulated analog ratemeter with auto ranging digital ratemeter in CPM or CPS count elapsed time preset count preset time high voltagesetting acquisition time and run number Data is loaded into spreadsheet compatible files for transfer Bi directional LABLINK offers full control of all functions including preset count preset time countrate in CPM or CPS alarm level high voltage start stop reset and data transfer Requires EGA or graphics All operations may be run directly from the computer with spreadsheet compatibility Table 3 1 This is a copy of the Specifications of the Spectech ST 350 system from the user manual http www spectrumtechniques com manuals ST350manual pdf Team CajunSat 51 FRR v3 0 Figure 3 10 Thi
91. te Poisson distribution function and Gaussian distribution function Repeat the procedure in the previous paragraph for the measurements in Section 4 5 with the source in the higher position In your report discuss the differences of the shapes of the Poisson and Gaussian distributions in of the two sets of measurements Also discuss the validity of approximating the Poisson distribution with the Gaussian distribution in each case Is the standard deviation of the higher count statistics equal to the square root of the mean number of counts Team CajunSat 56 FRR v3 0 6 1 3 Flux Calculations After finding the area of the Geiger counters dead time and voltage plateau we are finally able to find and compare the flux rate of flow per unit area of the cosmic rays We will do this by using the following flux formula counts Flux area x time The previous formula is the general formula for flux that does not include the dead time of the detector The following formula includes the dead time of the detector and will give us an accurate flux measurement Counts Flux Area X Time Dead time Because our area and time will be constant we can rewrite the flux formula in the following way Counts Flux 1 18 cm x Time Dead time This is for the K2645 Geiger counter while the next formula is for the LND 7232 Geiger Counter Counts Flux 6 88 cm x Time Dead time To calculate t
92. ters and Geiger Muller counter The heating problem can only be resolved by prototyping The question to address is how sufficient is a single 1 W ceramic resistor This will be accomplished by performing the same environmental testing as for all other components Both of these points are critical in determining the number of batteries needed for the payload and ultimately final payload mass The only other design issue is determining the accuracy of the Geiger counter This will be accomplished by testing the counter against known gamma sources and calculating the flux at sea level and comparing it to the known flux 5 1 1 Geiger Muller Counter K2645 The Geiger counter we will be using is the Geiger Muller counter K2645 kit created by Velleman Inc This kit provides an acoustic measurement of radiation levels The sensitivity is at its highest for gamma rays and high energy beta rays The assembly is compact and may be mounted into a small box together with the 9V battery The specifications are as follows Battery supply of 9V Maximum current of 200 Sensitive to gamma rays and high energy beta rays Dimensions are 54 x 99 x 25 mm ee Team CajunSat 47 FRR v3 0 5 Characteristics of tube have a tolerance of 10 Figure 3 14 Picture of our completed Geiger counter ER a IHi ET HH 1 See i E sii H E si H
93. the same 9V battery as the Geiger counter The 74C157 data selector allows the stamp to read 8 bits of the counter one nibble at a time The 9th bit is read by the stamp All other bits are discarded allowing up to 512 counts in a one minute period The A B selector on the 74C157 doubles as a serial output for the PC interface The Geiger counter reading is updated once per minute and is based on the total counts received from between one minute and four hours of operation The longer the device is operated the more accurate the readings will be The Stamp sends the minute by minute reading out as numeric data followed by a carriage return and line feed at 2400 Baud When the Stamp is turned on this data is immediately sent out through the serial port at 2400 Baud The data is sent numerically with a line feed and carriage return after each number the earliest measurement first Team CajunSat 36 FRR v3 0 WM Resister Wires Resistance 202 Battery Figure 4 7 a Circuit design of Heating Circuit Figure 4 7 b The heating Circuit design 4 4 Thermal Design We expect to encounter an environment with temperatures ranging from 60 C to 80 C The electrical components in our payload BASIC stamp Geiger counter etc have operating ranges of minimum 20 C to maximum 70 C The only problem this causes is maintaining the payloads temperature at 20 C at max altitude and min pressure If temperatu
94. ticles This is because alpha particles are stopped by a piece of paper Therefore our two layers of foam board will stop all alpha particles Beta particles and gamma rays on the other hand will not be stopped by the foam board because beta rays are stopped by a sheet of aluminum or plywood while gamma rays are stopped by a two meters of concrete or 40 cm of lead Reference 11 Figure 3 1 shows this better Team CajunSat 2 FRR v3 0 Sheet of Paper 1 Metre of Concrete Figure 3 1 This shows how far each particle can travel through a given object http www cameco com uranium_101 uranium_science radiation index php 3 1 1 Cosmic Rays Cosmic rays are particles that bombard Earth from anywhere beyond its atmosphere Reference 3 and were discovered by Victor Hess see figure 3 2 using a high altitude balloon traveling to about 17 500 feet 5 334 km and a gold leaf electroscope Reference 14 He noticed that the electroscope discharged more rapidly has we went up in altitude and attributed this as a form of radiation entering the atmosphere from above This discovery earned him a Nobel Prize in 1936 For a long time cosmic rays were considered electromagnetic in nature but during the 1930 s it was discovered that they are electrically charged and affected by things such as Earth s magnetic fields This means that the flux of the cosmic rays will be different at different latitudes and at different altitudes because Earth acts
95. ulk heating Bulld Geiger counter using Kit ens g Bi rco board mum g Design structural layout sum toas Lithium battery load check g Geiger counter rate check EA g Geiger counter accuracy check Karara AM TIN eee D FRR v3 0 74 Team CajunSat 9 3 Timeline and Milestones 3 1 2005 3 17 2005 3 31 2005 4 1 2005 4 13 2005 4 22 2005 5 1 2005 5 23 2005 5 25 2005 5 26 2005 6 1 2005 Team CajunSat 75 FRR v3 0 10 0 Master Budget Figure 10 1 Table of the costs Item Estimated Description Lead Time Pricing Comments Cost Lithium Batteries No wait time approximately producing 9V purchased at local 11 00 per 9V Parries 369 09 Batteries for actual flight retail store battery and for testing Used as a back up for the express shipment 1 of Lafayette Donated Velleman K2645 Geiger approximately 2 5 Scout 2 LaACES use no Muller Counter Kit day wait period cost to budget Velleman K2645 Used for detection of beta express shipment detailed Geiger 150 00 and gamma radiation in approximately 2 5 information 1s Muller final payload day wait period listed below Counter Kit Supplies for interfacing the approximately Additional BASIC STAMP to the No wat me 1 2 per item Supplies for Velleman K2645 Geiger used
96. upplies Built on 2 10 05 used for testing on a regular basis Heating Elements Purchased 3 24 05 Insulation Existing Supplies 3 24 05 f Existing Supplies Electrical Components Purchased 3 24 05 M E Existing Supplies Purchased 2 24 05 Existing Supplies Purchased as needed for the Tesung Supphes Purchased project Geiger Muller Counter Purchased 3 8 05 3 24 05 Gamma Scout Donated 3 3 05 3 24 05 Figure 10 3 Purchasing record Team CajunSat 78 FRR v3 0 11 0 Risk Management and Contingency In order for us to have a successful flight we must do lots of testing This ranges from cold testing vacuum testing impact testing and equipment testing The following section explains and gives results of the different testing we did 11 1 Stress testing The first test we did was a stress test of the box rolling it down a flight a stairs One thing that was noticed is that our only problem will be us securing our payload to the box We solved this by installing slits in the boxes The different slits will provide the stabilization at impact and will be able to survive just about any kind of impact except maybe a parachute failure We did not roll our slit design down the stairs but instead threw it our of a second story window See figure 11 2 Surprisingly there was very little damage to the outside of the box and only a broken piece of balsa wood and dented slit This is not a p
97. ups 10 front panel setups 3 5 in 1 44 MB or 720 K DOS compatible PC formats BMP Floppy Drive TIF PCX EPS spreadsheet formats Excel Lotus123 and MathCAD for mathematical modeling and analysis Table 11 10 This is a table of the non volatile storage of our oscilloscope http www tek com Measurement cgi bin framed pl Document Measurement Products catalog tds300 specs html amp FrameSet oscilloscopes Option 14 I O Interface Full talk listen modes Control of all modes settings and measurements Full talk listen modes Control of all modes RS 232 C Interface Programmability settings and measurements Baud Rate up to 38 400 9 Pin DTE Monitor output for direct display on large VGA equipped monitors GPIB IEEE 488 2 Programmability VGA Hardcopy Port Centronics type parallel RS 232 C or GPIB DC Power for Printer Programmer Manual 070 9442 00 Table 11 11 This is a table of the option 14 I O Interface of our oscilloscope http www tek com Measurement cgi bin framed pl Document Measurement Products catalog tds300 specs html amp FrameSet oscilloscopes Hard Copy Capability Graphics File Formats Interleaf 1mg TIF PCX PC Paintbrush BMP Microsoft Windows and Encapsulated PostScript EPS Printer Formats Thinkjet Deskjet Laserjet Epson 9 amp 24 Pin Seiko DPU 411 II DPU 412 DPU 414 Available Printer Packs
98. wing procedures Make sure balance is level Zero out the balance Place the object to weighed on the balance Weight until the balance comes go a general number within to about 0 020 g We cannot get an exact number because it will continue to fluctuate by about 0 020g because of environment We just add this fluctuation to the error with the balance error dub Team CajunSat 44 FRR v3 0 5 Take a picture of the weight to used as documentation 6 Record the weight Team CajunSat Component Weight g Electronics with 3 lithium 225 56 g batteries Inner box with balsa wood 90 10 g Outer box 89 8 g Foam inserts 12 09 Total weight 446 5 g Table 4 3 Table of the weights of each component with the error Some of the weights are pending 45 FRR v3 0 Weight budget breakdown Electronics with 3 lithium batteries Inner box Outer box Foam Figure 4 14 Weight Budget Breakdown Team CajunSat 46 FRR v3 0 Figure 4 12 A Weight of our outer box 5 0 Payload Development Plan The design for the circuitry involved is complete except for two major points We still need to do environmental testing for several components and we need to calibrate the Geiger counter Environmental testing requirements for the flight are 60 C and 7 6 Torr Both of these are approximations based on standard models and previous measurements All environment tests are complete except for the hea

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