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SMARTS code, version 2.9.5 USER`S MANUAL

1. CARD 8 AEROS AEROS selects the aerosol model with one of the following twelve possible choices S amp F_RURAL S amp F_URBAN S amp F_MARIT S amp F_TROPO These four choices refer respectively to the Rural Urban Maritime and Tropospheric aerosol models Shettle and Fenn 1979 which are humidity dependent and common with MODTRAN SRA_CONTL SRA_URBAN SRA_MARIT These three choices refer respectively to the Continental Urban and Maritime aerosol models of the IAMAP preliminary standard atmosphere IAMAP 1986 BED C B amp D Cl These two choices refer respectively to the Braslau amp Dave aerosol type C and Cl themselves based on Deirmendjian s Haze L model DESERT MIN DESERT_MAX These two choices are new in version 2 9 5 DESERT_MIN corresponds to background normal conditions in desert areas whereas DESERT_MAX corresponds to extremely turbid conditions sand storms The optical characteristics of all these default aerosol models are calculated by the program from wavelength as well as relative humidity in the case of the Shettle amp Fenn aerosols USER This last option is to be used if none of the above default aerosol model is appropriate i e to describe realistic as opposed to ideal conditions Card 8a is then necessary to input user supplied aerosol information 15 CARD 8a if AEROS USER ALPHA1 ALPHA2 OMEG
2. TRL Tropical STS Sub Tropical Summer STW Sub Tropical Winter AS Arctic Summer AW Arctic Winter Note 1 Only the 6 first atmospheres are available in LOWTRAN or MODTRAN Note 2 The reference atmospheres determine pressure temperature relative humidity ozone and precipitable water in the free atmosphere at the total altitude specified on Card 2 ALTIT HEIGHT If this altitude is gt 0 the reference atmospheres will consider the site as an aircraft or a very tall tower i e will not consider any boundary layer effect which tends to increase temperature relative humidity and precipitable water For better results at most sites it is preferable to define a non reference atmosphere on Card 3 and specify precipitable water on Card 4 and ozone on Card 5 CARD 4 IH20 IH20 is an option to select the correct water vapor data All water vapor calculations involve precipitable water W The following values of IH20 are possible 0 to input W on Card 4a 1 if W is to be defaulted to a value prescribed by the selected reference atmosphere and the site altitude thus if IATMOS 1 on Card 3 If ATMOS 1 USSA will be defaulted for this step 2 if W is to be calculated by the program from TAIR and RH thus if IATMOS 0 on Card 3 This calculation is only approximate particularly if HEIGHT gt 0 and therefore this option is not recommended 10 CARD 4a if IH20 0 W W is precipitabl
3. LATIT Site s latitude decimal degrees positive North negative South e g 17 533 for Papeete Tahiti If LATIT is unknown enter 45 0 ALTIT Site s altitude i e elevation of the ground surface above sea level km must be lt 100 km In case of a flying object ALTIT refers to the ground surface below it HEIGHT Height of the simulated object above the ground surface underneath km must be lt 100 km new input The total ALTIT HEIGHT is the altitude of the simulated object above sea level and must be lt 100 km Note 1 If ISPR 1 on Card 2 SPR is used as the main input for all pressure related calculations To study the effect of varying altitude through ALTIT or HEIGHT on irradiance it is therefore imperative to use one of the following two options i use ISPR 2 forcing SPR to be recalculated each time ALTIT or HEIGHT varies or ii use ISPR 1 but each time ALTIT or HEIGHT varies provide the re evaluated SPR that corresponds to the effective altitude ALTIT HEIGHT Note 2 If ISPR 2 on Card 2 and IATMOS on Card 3 the default SPR value generated by the reference atmosphere will ultimately replace the estimate from ALTIT and LATIT based on Card 2a information CARD 3 IATMOS IATMOS is an option to select the proper default atmosphere Its value can be either 0 or 1 Set IATMOS 0 to define a realistic i e non reference atmosphere Card 3a will then have to provide TAIR RH SEASON TDAY
4. Set IATMOS to select one of 10 default reference atmospheres i e for ideal conditions The shortened name of this atmosphere must be provided by ATMOS on Card 3a If ATMOS 0 is selected then IH20 should be 0 or 2 I03 and IGAS should be 0 If IATMOS is selected then IH20 I03 and IGAS may take any value All user inputs have precedence over the defaults CARD 3a if IATMOS 0 TAIR RH SEASON TDAY RH Relative humidity at site level SEASON Can be either WINTER or SUMMER for calculation of precipitable water and stratospheric temperature If the true season is Fall select WINTER Select SUMMER if the true season is Spring SEASON slightly affects the ozone effective temperature and the aerosol optical characteristics TAIR Atmospheric temperature at site level C Acceptable range 120 lt TAIR lt 50 TDAY Average daily temperature at site level C For a flying object HEIGHT gt 0 this is a reference temperature for various calculations therefore it is important to provide a realistic value in this case in particular Acceptable range 120 lt TDAY lt 50 CARD 3a if IATMOS 1 ATMOS neces OE ates ATMOS is the name of the selected reference atmosphere 4 characters max This name can be one of the following USSA U S Standard Atmosphere MLS Mid Latitude Summer MLW Mid Latitude Winter SAS Sub Arctic Summer SAW Sub Arctic Winter
5. PRINTOUTS FOR EXAMPLE 6 e INPUT FILE Example_6 USSA_AOD_0 084 1 1013 25 0 0 1 USSA 1 1 1 370 0 0 S amp F_RURAL 0 0 084 38 1 38 37 180 280 4000 1 0 1367 0 2 280 4000 5 4 89 10 30 1 02 90 0 0 0 2 1 5 Card 1 Comment Card 2 ISPR Card 2a Pressure altitude height Card 3 IATMOS Card 3a Atmos Card 4 TH20 Card 5 103 Card 6 IGAS Card 7 qCO2 Card 7a ISPCTR Card 8 Aeros Card 9 ITURB Card 9a Turbidity coeff TAUS Card 10 IALBDX Card 10b ITILT Card 10c Tilt variables Card 11 Input wavelengths solar spectrum Card 12 IPRT Card12a Print limits Card12b Variables to Print Card12c Variable codes Card 13 ICIRC Card 13a Receiver geometry Card 14 ISCAN Card 15 ILLUM Card 16 IUV Card 17 IMASS Card 17a Air mass 49 e OUTPUT FILE Ti ok oi ok ok ak ok ok ak ak ok kK SMARTS version 2 9 5 22 278 2 2 kkk kk kk K KK K K A J Simple Model of the Atmospheric Radiative Transfer of Sunshine Chris A Gueymard Solar Consulting Services December 2005 This model is documented in FSEC Report PF 270 95 and in a Solar Energy paper vol 71 No 5 325 346 2001 NOTE These references describe v 2 8 or earlier See the User s Manual for details on the considerable changes that followed DiS AS FAS 2S E E AS E E K K K K E K K K K K K K K K K K KK K K K K K K K K K K KK K K K K KK K K K KK K 2K K K 2 2 K K 2s 2 OK K K Reference for t
6. no the previous message reappears and the cycle continues until you reply yes The output files will be located in the same folder as the input file e g in the INPUT folder for this example For convenience a Terminal window size of at least 120x36 is recommended this size can be saved for future use in the Terminal Preferences To use any sample input file contained in one of the subfolders within the Examples folder move it to the root of the SMARTS_295 Mac folder thus replacing any pre existing file of the same name However before undertaking the execution of any new run using an input file with the same name it is imperative to either rename the existing output files or to move them to the OUTPUT folder or any other folder Failing to do so would prevent proper execution and generate the following error message open new fil xists apparent state unit 17 named smarts295 ext txt last format list io lately reading sequential formatted external IO SCIENCE SMARTS 295 Mac smarts295 command line 3 15256 Abort trap Source_code smarts295_cmd logout Process completed Power users can change this feature by altering the appropriate OPEN statements in the Fortran code so that at anytime they are overwritten and by recompiling The source code smarts295 f resides in the Source_Code folder and can be compiled with any Fortran77 compiler An open source free Fortran compiler g77 is available
7. 9 to 2 9 2 Options 2 7 are directly derived from the six high resolution spectra selectable in MODTRAN 4 0 and thus allow better compatibility with any irradiance prediction obtained with this code Option 1 NEW is for a user defined spectrum to be read in file Spctrm_U dat This file is originally a copy of Spctrm_O dat but can be altered by the user inasmuch as the original format wavelengths and units are conserved See Section 8 for more details Option 8 NEW is for an interpolated version of the ASTM E490 standard spectrum ASTM 2000 It has been specially prepared by Daryl Myers for those applications that require compliance with this ASTM standard See Section 13 and Gueymard 2004 for more details and intercomparisons between the solar spectra offered here 14 Cotton File an 4 Source a w 1 Spctrm_U dat N A User User 0 Spctrm_0 dat N A Gueymard 2004 synthetic 1366 10 1 Spctrm_1 dat N A Gueymard unpublished synthetic 1367 00 2 Spctrm_2 dat cebchkur MODTRAN Cebula Chance Kurucz 1362 12 3 Spctrm_3 dat chkur MODTRAN Chance Kurucz 1359 75 4 Spctrm_4 dat newkur MODTRAN New Kurucz 1368 00 5 Spctrm_5 dat oldkur MODTRAN Old Kurucz 1373 16 6 Spctrm_6 dat thkur MODTRAN Thuillier Kurucz 1376 23 7 Spctrm_7 dat MODTRAN2 Wehrli WRC WMO 1985 1367 00 8 Spctrm_8 dat N A ASTM E490 2000 synthetic 1366 10
8. Af a X a a A have been revised to take new fundamental determinations into account Bucholtz 1995 Bodhaine et al 1999 The functional form above guarantees a significantly better fit to the theoretical data than the polynomial ratio recommended by Bodhaine et al e Revised optical masses Each extinction process has now a separate optical mass obtained as a function of zenith angle The air mass takes the atmosphere s curvature and the vertical profile of each absorber or scatterer into account and thus alleviates the limitations of the usual plane parallel approximation New absorption coefficients All absorption coefficients are either new or revised in this version and are based on the latest spectroscopic data There is now a total of 19 absorbing gases a number of them new to SMARTS some of them not considered in MODTRAN yet Wherever possible the absorption coefficients are temperature dependent All gases are treated individually with a separate input data file hence the far larger number of data files in the present version e Pollution mode 44 The abundance of all gases is defaulted to standard conditions calculated from pressure and temperature The abundance of those 10 gases that are highly variable due to tropospheric pollution e g O NO SO can be modified with a pollution index Their real tropospheric abundance can be either user defined in ppm or defaulted to four representati
9. Denver s International Airport Colorado ZONE International Time Zone relative to Greenwich with the same sign convention as LONGIT e g ZONE 5 for Eastern Standard Time North America ZONE 2 for Greece The Local Apparent Time LAT corresponding to the input s Local Standard Time LST is calculated and printed to the main output file smarts295 out txt or File 16 However for some applications it might be necessary to relate to LAT rather than Local Standard Time LST as used here Predicting irradiances exactly at solar noon i e 12 00 LAT is a typical example Such a calculation is possible but requires a preliminary run where HOUR would be set to 12 From the LAT value that is printed on File 16 it is easy to obtain the difference between LAT and LST The final run would be done after adjusting HOUR for this difference When IMASS 3 the actual sun earth distance is calculated from the supplied date and overwrites the SUNCOR value from Card 11 27 CARD 17a if IMASS 4 MONTH LATIT DSTEP MONTH Any integer between 1 and 12 LATIT Site latitude decimal degrees positive North negative South e g 17 533 for Papeete Tahiti DSTEP Time interval min for the numerical integration of irradiation when a daily calculation is requested DSTEP must be a real number and divisor of 60 hence this non exhaustive list of possible values of DSTEP 1 2 3 4 5 6 7 5 10 12 15 20 30 60 DS
10. The two series of broadband results that are provided for the 400 700 nm spectral range are the photosynthetic irradiance W m and the photosynthetic photon flux density umol m s CARD 16 IUV IUV Option for special broadband UV calculations Select IUV O for no special UV calculation IUV 1 to initiate such calculations These include UVA UVB UV index and different action weighted irradiances of interest in photobiology Note that IUV 1 overrides WLMN and WLMX so that calculations are done between at least 280 and 400 nm The spectral results are also printed between at least 280 and 400 nm irrespective of the IPRT WPMN and WPMX values CARD 17 IMASS IMASS Option for solar position and air mass calculations Set IMASS to O if inputs are to be ZENIT AZIM on Card 17a 1 if inputs are to be ELEV AZIM on Card 17a 2 if input is to be AMASS on Card 17a 3 if inputs are to be YEAR MONTH DAY HOUR LATIT LONGIT ZONE on Card 17a 4 if inputs are to be MONTH LATIT DSTEP on Card 17a for a daily calculation CAUTION The option IMASS 2 does not completely define the sun s position therefore the sun s azimuth is defaulted to 180 0 south facing If tilted irradiance calculations are necessary ITILT 1 it is better avoiding the IMASS 2 option However a tracking surface can be simulated with this option without problem 26 CARD 17a if IMASS 0 ZENIT AZIM ZENIT Apparent solar zenith
11. atmosphere hence the negative values for the additional concentrations 12 Gas 1 Pristine 2 Light Pollution 3 Moderate 4 Severe CH O 0 003 0 001 0 007 0 01 CH 0 0 2 0 3 0 4 CO 0 1 0 0 35 9 9 HNO 9 9E 4 0 0005 0 002 0 01 HNO 0 0 001 0 005 0 012 NO 0 0 075 0 2 0 5 NO 0 0 005 0 02 0 2 NO 4 9E 4 1E 5 SE 5 2E 4 O 0 007 0 023 0 053 0 175 SO 0 0 01 0 05 0 2 CARD 6b Gf IGAS 0 and ILOAD 0 ApCH20 ApCH4 ApCO ApHNO2 ApHNO3 ApNO ApNO2 ApNO3 ApO3 ApSO2 ApCH20 Formaldehyde volumetric concentration in the assumed 1 km deep tropospheric pollution layer ppmv ApCH4 Methane volumetric concentration in the assumed 1 km deep tropospheric pollution layer ppmv ApCo Carbon monoxide volumetric concentration in the assumed 1 km deep tropospheric pollution layer ppmv Card 6b ApHNO2 Nitrous acid volumetric concentration in the assumed 1 km deep tropospheric pollution layer ppmv ApHNO3 Nitric acid volumetric concentration in the assumed 1 km deep tropospheric pollution layer ppmv ApNO Nitric oxide volumetric concentration in the assumed 1 km deep tropospheric pollution layer ppmv ApNO2 Nitrogen dioxide volumetric concentration in the assumed 1 km deep tropospheric pollution layer ppmv ApNO3 Nitrogen trioxide volumetric concentration in the assumed 1 km deep tropospheric pollution layer ppmv ApO3 Ozone volumetric concentration in the assum
12. followed the content of each of these files is copied to the default input file with the help of the cp command copy Then the smarts295script executable reads this input file make the appropriate calculations and pass the output to the default files In order not to overwrite the default output files they are renamed with the help of the mv command move Once the end statement is reached the foreach command will move to the next argument If all arguments are used the user will be returned to the standard prompt It is clear that the user can change the arguments of the foreach command to suit his her needs All text files and the executable are assumed to reside in the root directory of the code 4 4 Compiler issues Commercial Fortran compilers are generally more powerful than g77 Therefore the executables provided here might not be the fastest possible See http hpc sourceforge net for OSX optimization tools This is not a problem in normal use because execution takes only a few tenths of a second For extremely intensive batch jobs e g thousands of chained runs at a time it would be advisable to recompile the code with one of these high performance compilers An example of extremely intensive use of SMARTS is in the mesoscale radiation analysis project STRANG http produkter smhi se strang Another issue is that compilers may not interpret code the same way depending on user define
13. http www gnu org software fortran fortran html It may be installed in various ways for instance through the combined use of Fink http fink sourceforge net and Xcode http developer apple com tools xcode index html which can be both obtained freely Once g77 is installed the Terminal command g77 o smarts295 03 fdollar ok w smarts295 f should complete without any errors and create an optimized executable called smarts295 Note that there is no space before ok and the O3 option uses a capitalized O Finally move or copy this new executable to the SMARTS_295_ Mac folder 4 2 Command line execution In command line or batch mode the program runs without user interaction It assumes that the correct input file is smarts295 inp txt at the root of the main folder To run the Command Line executable smarts295bat from the Terminal type cd SMARTS 295 Mac smarts295bat and hit Enter after each line This first message appears KKK KKK KEK KKK KKK KK KKK KKK KKK KKK KK KKK KK Welcome to SMARTS version 2 9 5 KKK KKK KK KK KKK KKK KKK KKK KKKKK KKK KK KKK and when the program stops a final message similar to this one is displayed Total CPU time 0 190 sec Solar SCIENCE SMARTS 295 Mac chris Execution of the sample input file must have created two output files smarts295 out txt and smarts295 ext txt at the root of the main folder To avoid
14. in Section 6 Save it as TEXT Unix format with the same filename or any other name of your choice in the format any_file_name inp txt e g Test_for_July inp txt Note that the default input filename is smarts295 inp txt and remember that filenames are case sensitive if the program is invoked from a Unix shell e g with Terminal 4 1 Standard execution To run the Standard executable described in Section 2 double click on the smarts295 file whose icon is based on the SMARTS logo and whose name may alternatively appear as smarts295 command if the Finder Preferences are set to Show all file extensions This will launch the executable smarts295_cmd located in the Source_code folder and open a single use Terminal window A welcome message appears KKK KKK KKK KKK KEK KK KKK KKK KKK KKK KK KK KKK Welcome to SMARTS version 2 9 5 KEKE KK KK KK KK KK KKK KKKKK KK KAKA KK KK KKK SMARTS 295 gt Use standard mode with default input file If YES or Y execution will start immediately using the default input file smarts295 inp txt Y N gt e If you type y or yes and hit Enter execution begins immediately A final message similar to this one is displayed when execution ends Total CPU time 0 190 sec logout Process completed The Terminal window s name becomes Completed Command at which point it can be closed Execution of the preloaded sample input file m
15. index for skin cancer incidence Proc 3rd Conf on CIAP DOT TSC OST 74 15 Department of Transportation Washington DC 46 Green A E S and Mo T 1975 Erythema radiation doses in Impacts of climatic change on the biosphere D S Nachtwey et al eds CIAP Monograph 5 DOT TST 75 55 Part 1 Chapter 2 Department of Transportation Washington DC Green A E S Sawada T and Shettle E P 1974 The middle ultraviolet reaching the ground Photochem Photobiol 19 251 259 Gueymard C 1994a Analysis of monthly average atmospheric precipitable water and turbidity in Canada and Northern United States Solar Energy 53 57 71 Gueymard C 1994b Updated transmittance functions for use in fast spectral direct beam irradiance models Proc Solar 94 Conf ASES San Jose CA pp 355 360 Gueymard C 1995 SMARTS2 Simple Model of the Atmospheric Radiative Transfer of Sunshine Algorithms and performance assessment Rep FSEC PF 270 95 Florida Solar Energy Center Cocoa FL Gueymard C 1998 Turbidity determination from broadband irradiance measurements A detailed multicoefficient approach J Appl Meteorol 37 414 435 Gueymard C 2001 Parameterized Transmittance Model for Direct Beam and Circumsolar Spectral Irradiance Solar Energy 71 325 346 Gueymard C 2004 The sun s total and spectral irradiance for solar energy applications and solar radiation models Solar Energy 76 423 453 Gueymard C 2005 Interdisciplinar
16. latitudel lt 85 deg The input data for this day are such that Ideclination latitudel deg RUN ABORTED Daily calculations can only be done if the sun is high enough during the average day of the month 7 Value of ZENIT is gt 90 deg RUN ABORTED Calculations can only be done during sunup hours See Card 17a 8 Value of AMASS is gt 38 2 RUN ABORTED Calculations can only be done during sunup hours See Card 17a 33 11 SAMPLE RUNS AND PRINTOUT Sample runs are provided and reside in separate Example folders directories Each one is documented with a ReadMe file The input and output files are provided so that the user can test if his her results are in complete agreement with these sample runs The printouts of files SMARTS295_INP txt and SMARTS295_OUT txt corresponding to the particular case described in Example 6 of this package appear in the Appendix for reference purposes k IMPORTANT NOTE Example 6 allows to approximate the most recent reference spectra at air mass 1 5 adopted in 2003 by ASTM under standard G173 03 which was based on version 2 9 2 of this code 12 UV ACTION WEIGHTED IRRADIANCES Extra UV calculations are invoked when the option IUV is set to 1 For each wavelength the global horizontal irradiance is then convolved with a specific biological action spectrum When summed over all UV wavelengths this provides an action weighted irradiance which can be of intere
17. on Card 9a must correspond to the aerosol total column between the receiver s altitude and the top of the atmosphere This may represent a challenge when dealing with an aircraft based receiver for instance due to the lack of data at high altitude For a receiver at altitudes above about 6 km it is possible to obtain TAU550 from the effective altitude z i e ALTIT HEIGHT in km by using the following empirical relationship T559 exp 3 2755 0 15078 z 16 If BETA is not input all possible alternatives BCHUEP RANGE TAU5 TAU550 VISI are converted by the program first to J then to a spectral aerosol optical depth T by use of equations such as T 2 302585 B f 0 5 2 T 0 552 Taso Vp 1 306 V T B 0 5 192 AA if A lt 0 5 um t fA if A 20 5 um B 00 55 2 CVa In the special case when IATMOS and AEROS S amp F_RURAL however 1 is evaluated with Angstr m s e uation T k where ais obtained as a stepwise fit of the original data 8 q an p g in Shettle and Fenn 1979 If this particular calculation does not appear appropriate either set IATMOS to 0 rather than 1 to define a USER atmosphere with AEROS S amp F_RURAL or set AEROS USER to define a user aerosol along with IATMOS 1 CARD 10 taLBpx IALBDX is an option to select the correct zonal or far field albedo RHOX for backscattering calculations From the reflectance standpoint the ground surfac
18. relative to MODTRAN W m nm 300 500 700 900 1100 1300 1500 1700 Wavelength nm Fig 6 Absolute difference between the direct irradiance predicted by SMARTS 2 9 BRITE as per the ASTM G159 standard tabulations and MODTRAN 4 0 15 APPLICATIONS Because of its versatility SMARTS can be used in a large number of applications covering a broad spectrum of activities A detailed review is available elsewhere Gueymard 2005 One of these applications in particular is worth mentioning here because of its long term impact Following the development of SMARTS based reference spectra Gueymard et al 2003 the American Society for Testing and Materials ASTM has recently adopted these reference spectra to replace those in the existing G159 standard mentioned in Section 14 Another reference high UV global spectrum has also been standardized The two new spectra and the new UV spectrum in these standards G173 03 and G177 03 respectively are specifically based on version 2 9 2 of the code It will be kept in a frozen state for permanent reference even if new updates continue to be developed leading to slightly different results for identical conditions like in the present case ASTM also plans to offer version 2 9 2 as an adjunct standard on CD ROM Please refer to http www astm org and http rredc nrel gov solar models SMARTS for further information 41 16 SUMMARY OF NEW FEATURES IN VERSION 2 9 x Vers
19. teacher ozone_overhead html and GOME http www knmi nl gome_fd tm3 lvl4 html or from ground based spectrophotometers from the WOUDC network http www woudc org data_e html 11 Most measured total column data in the present era are expressed in Dobson units DU 1000 Dobson units are equivalent to 1 atm cm AbO3 represents the total column abundance of ozone above site level It may be corrected by the program if IALT is set to 1 A correction with altitude is then applied to AbO3 so that the apparent ozone column from an elevated site can be obtained from available sea level data Tropospheric ozone may be present in polluted areas but it is normally a small fraction of the total ozone Reference atmospheres indicate a sea level ozone concentration of 0 018 0 030 ppmv If the site s ozone concentration is appreciably higher and is known to be excluded from the columnar abundance specified by AbO3 SMARTS has an option to take this additional contribution into account through ApO3 see Cards 6 and 6a CARD 6 IGAS IGAS is an option to define the correct conditions for gaseous absorption and atmospheric pollution IGAS 0 if ILOAD on Card 6a is to be read so that extra gaseous absorption calculations corresponding to the gas load in the lower troposphere due to pollution or absence thereof can be initiated IGAS 1 if all gas abundances except carbon dioxide ozone and water vapor see Cards 4a Sa and 7 a
20. this author Two other results are further obtained from the CIE erythemal irradiance The UV dose in MED hr where 1 MED 210 J m is calculated to simulate the output of a Robertson Berger biometer Finally the UV index which is now used regularly in many meteorological reports and forecasts for public protection purposes is obtained as 40 times the erythemal irradiance Note that previous versions of SMARTS have been used in different countries to predict the UV index Koepke et al 1998 Lehmann 2001 34 13 REVISED EXTRATERRESTRIAL SPECTRUM A significant revision of the extraterrestrial spectrum is now proposed and recommended It has been obtained as a synthesis from the most recent sources using data with the least uncertainty possible and appropriate corrections Gueymard 2004 This new spectrum covers the region 0 5 nm to 1000 ym and integrates to 1366 1 W m the currently accepted value of the solar constant Figure 2 shows how the newly proposed spectrum compares to other existing spectra namely the previous SMARTS spectrum Gueymard 2002 unpublished the newer Kurucz spectrum used in MODTRAN newkur and the ASTM standard ASTM 2000 The Kurucz spectrum integrates to 1368 0 W m whereas the ASTM spectrum integrates to 1366 1 W m like the newly proposed spectrum Note that the IR part of all these spectra are based on a version or another of the Kurucz spectrum hence their good agreement there no
21. 0 4 4 0 S 32 Lightloam LiteLoam NL 0 431 4 0 S 33 Light sand LiteSand NL 0 4 4 0 S 34 Pale loam PaleLoam NL 0 4 4 0 S 35 Sea water Seawater NL 2 079 4 0 W 36 Solid ice SolidIce NL 0 3 4 0 W 37 Dry soil Dry_Soil NL 0 28 4 0 S 38 Light soil LiteSoil NL 0 28 4 0 S 39 Old runway concrete RConcrte NL 0 3 4 0 M 40 Terracota roofing clay tile RoofTile NL 0 3 4 0 M 41 Red construction brick RedBrick NL 0 3 4 0 M 42 Old runway asphalt Asphalt NL 0 3 4 0 M 43 Tall green corn TallCorn NL 0 36 1 0 V 18 44 Sand amp gravel SndGravl NL 0 45 1 04 S 45 Fallow field Fallow NL 0 32 1 19 S 46 Birch leaves Birch NL 0 36 2 48 V 47 Wet sandy soil WetS Soil NL 0 48 2 48 S 48 Gravel Gravel NL 0 32 1 3 S 49 Wet red clay WetClay2 NL 0 52 2 48 S 50 Wetsilt WetSilt NL 0 52 2 48 S 51 Dry long grass LngGrass NL 0 277 2 976 V 52 Lawn grass generic bluegrass LwnGrass NL 0 305 2 944 V 33 Deciduous oak tree leaves OakTree NL 0 35 2 5 V 54 Pinion pinetree needles Pinion NL 0 301 2 592 y 55 Melting snow slush MeltSnow NL 0 35 2 5 W 56 Plywood sheet new pine 4 ply Plywood NL 0 35 2 5 M 57 White vinyl plastic sheet 0 15 mm WiteVinl NL 0 35 25 M 58 Clear fiberglass greenhouse roofing FibrGlss NG 0 35 2 5 M 59 Galvanized corrugated sheet metal new ShtMetal NL 0 35 2 5 M 60 Wetland vegetation canopy Yellowstone Wetland NL 0 409 2 478 V 61 Sagebrush canopy Yellowstone SageBrsh NL 0 409 2 478 V 62 Fir trees Colorado FirTrees NL 0 353 2 592 V 63 Coastal s
22. 3 6b IGAS 6 qco2 7 WPMN 12a ApO3 6b IH20 4 RANGE 9a WPMX 12a ApSO2 6b ILLUM 15 RH 3a wv1 14a ATMOS 3a ILOAD 6a RHOG 10d wv2 14a AZIM 17a IMASS 17 RHOX 10a YEAR 17a BCHUEP 9a INTVL 12a SEASON 3a ZENIT 17a BETA 9a I03 5 SLOPE 13a ZONE 17a 28 8 USER DEFINED DATA FILES Albedo data in File 19 Albedo dat located in the Albedo subfolder are user modifiable but need to follow a specific format This file must contain two columns and any number of rows up to a maximum of 3000 up from 2002 in previous versions and must be saved as TEXT These two columns are respectively for Wavelength wm Reflectance 0 0 to 1 0 A hard return is needed at the end of the last row otherwise the file might be read incorrectly Similarly the extraterrestrial spectrum data in File 15 Spctrm_U dat located in the Solar subfolder are now user modifiable They need to respect the same format and units as all other similar files Spctrm_n dat No interpolation or extrapolation is performed on the spectrum so the irradiance values may be changed but not their wavelength attribution This file must therefore contain 2002 spectral values from 280 to 4000 nm and must terminate with a hard return 9 OUTPUT FILES The OUTPUT to File 16 e g smarts295 out txt is well documented and thus self explanatory It gives an echo of the input data as well as a series of results from the spectral and broadband calcu
23. ELATIVE OPTICAL MASSES Rayleigh 1 500 Water Vapor 1 501 Ozone 1 498 NO2 1 500 Aerosols 1 501 CO2 Mixing Ratio at sea level ppmv 370 0 Total column abundances atm cm for all gases except H2O and for normal standard conditions BrO CH20 CH4 CINO3 CO CO2 HNO2 HNO3 NH3 0 2500E 05 0 3000E 03 0 1325E 01 0 1200E 03 0 8859E 01 0 2970E 03 0 1000E 03 0 3637E 03 0 175 1E 03 NO NO2 NO3 N2 N20 02 03 04 SO2 0 3145E 03 0 2044E 03 0 5000E 04 0 3827E 06 0 2473E 00 0 1678E 06 0 3438E 00 0 1678E 06 0 1 100E 03 ANGLES deg FOR TILTED SURFACE CALCULATIONS Surface Tilt 37 000 Surface Azimuth from North 180 000 Incidence Angle 11 236 Diffuse irradiance ratios tilted plane horizontal 0 8993 isotropic approximate conversion for reference 1 2420 anisotropic conversion model used here X CK k Ck CK CK k kK OK kK k kK CK OK CK OK kK kK k CK KR kK kK K k xK kK K KK OK OK SPECTRUM Total 0 100 um Extraterrestrial Irradiance used here 1367 00 W m2 i e 1 0000 times the selected solar constant 1367 00 W m2 due to the actual Sun Earth distance Source for selected solar spectrum Gueymard_2004 To account for the chosen Solar Constant value the selected solar spectrum has been uniformly multiplied by this scaling coefficient 1 0007 Wavelength Range 280 0 to 4000 0 nm Number of Wavelengths 2002 BROADBAND IRRADIANCES W m2 DIRECT BEAM AT NORMAL INCIDENCE Extraterrestrial 1348 92 T
24. L GG ALPHA Average value of Angstr m s wavelength exponent for wavelengths lt 500 nm generally between 0 0 and 2 6 ALPHA2 Average value of Angstr m s wavelength exponent for wavelengths gt 500 nm generally between 0 0 and 2 6 OMEGL Aerosol single scattering albedo generally between 0 6 and 1 0 GG Aerosol asymmetry parameter generally between 0 5 and 0 9 CAUTION These 4 variables must represent broadband average values only CARD 9 ITURB ITURB is an option to select the correct turbidity data input The different options are 0 to read TAUS on Card 9a 1 to read BETA on Card 9a 2 to read BCHUEP on Card 9a 3 to read RANGE on Card 9a 4 to read VISI on Card 9a 5 to read TAU550 on Card 9a new option CARD 9a if ITURB 0 TAU5 TAU5 Aerosol optical depth at 500 nm T CARD 9a if ITURB 1 BETA BETA ngstr m s turbidity coefficient i e aerosol optical depth at 1000 nm CARD 9a if ITURB 2 BCHUEP BCHUEP Schiiepp s turbidity coefficient B i e decadic aerosol optical depth at 500 nm CARD 9a if ITURB 3 RANGE RANGE Meteorological range Vp based on Koschmieder s equation must be between and 999 km CARD 9a if ITURB 4 VISI VISI Prevailing visibility V as observed at airports must be between 0 77 and 764 km CARD 94 if rruRB 5 TAU550 TAU550 Aerosol optical depth at 550 nm T5509 All values appearing
25. N 320 5 WPMX 1100 INTVL Interval for printing spectral results on Files 16 and 17 21 Example 1 if INTVL 0 5 the effective interval used by the program will automatically adapt to the maximum possible resolution in each spectral region 0 5 nm 280 400 nm 1 nm 400 1700 nm and 5 nm 1705 4000 nm Example 2 if INTVL is set to 2 nm the effective interval will be 2 nm 280 1702 nm and 5 nm 1705 4000 nm Example 3 if INTVL is set to 10 nm the effective interval will be 10 nm for all possible bands 280 4000 nm CARD 12b if IPRT 2 or 3 IOTOT IOTOT is the total number of output variables to print on File 17 it must be between 1 and 43 new up from 32 in version 2 9 2 A code defining these variables is read on Card 12c Variables will be printed in the order selected CARD 12c if IPRT 2 or 3 IOUT IOUT is a code number 1 43 to select the spectral variables to print on File 17 This code is to be selected among the following list 22 IOUT Output variable OmAANINDNFPWN RK 10 11 127 13 14 15 16 17 18 19 20 21 22 23 24 25 26 27 28 29 30 31 32 ad 34 ae 36 a 38 39 40 41 42 43 Extraterrestrial spectrum Direct normal irradiance Diffuse horizontal irradiance Global horizontal irradiance Direct horizontal irradiance Direct tilted irradiance Diffuse tilted irradiance Global tilted irradiance Experimental direct normal irradiance wi
26. OX Zonal broadband Lambertian ground albedo for backscattering calculations must be between O and 1 Observed values are usually between 0 12 and 0 60 See also the discussion about RHOG for Card 10d below CARD 10b ITILT ITILT is an option for tilted surface calculations Select ITILT 0 for no such calculation ITILT to initiate these calculations using information on Card 10c k CARD 10 if ITILT 1 IALBDG TILT WAZIM IALBDG is identical to IALBDX see Card 10 except that it relates to the foreground local albedo seen by a tilted surface The list of options is identical to that of IALBDG and thus extends from 1 to 64 new TILT Tilt angle of the receiving surface O to 90 decimal deg e g 90 0 for a vertical plane Use 999 for a sun tracking surface WAZIM Surface azimuth 0 to 360 decimal deg counted clockwise from North e g 270 deg for a surface facing West Use 999 for a sun tracking surface CARD 10d if ITILT 1 and IALBDG 1 RHOG RHOG Local broadband Lambertian foreground albedo for tilted plane calculations Card 10d Gf IALBDG 1 usually between 0 05 and 0 90 Under realistic conditions RHOX on Card 10a is generally different from RHOG on Card 10d Both may have large seasonal variations at high latitudes and in cold regions due to snow The difference between RHOG and RHOX may seem subtle they are frequently but incorrectly used interchangeably in the literature RHOX c
27. SMARTS code version 2 9 5 For Mac OSX USER S MANUAL SMARTS Christian A Gueymard Solar Consulting Services USA December 2005 revised August 2006 CONTENTS 1 INTRODUCTION ccccssssssscscssssssssssscesssscsssessssssssessssssssasessesseacessessessessssscssssssssassssssssssssssssscsasassnsssasasossssssacessssssacessesees 2 2 FORTRAN LANGUAGE AND EXECUTABLES ssesessesessessoseseoseseosessoscssoscseoscsroscseososeoeoseseoscseoseseoseseoscseoseseoeessoses 2 3 HARDWARE AND SOFTWARE REQUIREMENTS scccsssssssssssssssssssscssssssssssssssssscssssssssssssasessesssasessesssasessesees 3 4 SOFTWARE INSTALLATION AND USE seseseeseseoseoecseososeososeseoseseosessoseseosessoscssoscseososeoscseososessoseseosessoseseoseseeeeseeees 3 5 RUNNING THE CODE sseseseseosescoscseoscseoscseoscssoscseososeesoseoeosessosessosessoscsrosessoseseoeossoroseeeoseesoseesosessosessoseseoseseosessoseseeeoseese 7 6 INPUT PREPARATION sssesesseseosessosessoscseoseseoscseoscseososeososeseoseososeseorcseoscseoroseeeoseeeoseeroseesoseososessosessosessosesrosessoseseoseseoseseese 7 7 INPUT VARIABLES LIST sesssseseoseseoseseoseseosessoseseoseseoscseoscssoscseoscseseoseseoseseoseseoscseoecseosessosessosessosesroseseososeoscssososeseosesse 28 8 USER DEFINED DATA FILES cccssssssssossssssscssssssssssessssssssessssssssssssesssssesessssssosssessssosasessssssassssesssasessssssasesosssoares 29 9 OUTPUT FILES A E A E 29 10 TROUBLESHOOTING WARNING am
28. TEP lt 6 is recommended for better accuracy whereas DSTEP 15 is recommended for speedier results Tests have indicated that no real improvement in accuracy is obtained when DSTEP lt 5 Because of the large quantity of calculations involved with this daily option only broadband results are output irrespective of the value of IPRT on Card 12 eS IMPORTANT NOTES e As many 17a cards can be piled up as desired the program will perform the spectral calculations sequentially All other variables remain constant during these successive runs e It is recommended to insert a blank line after the last input card or that card might not be read 7 INPUT VARIABLES LIST For cross reference purposes all possible input variables are listed below in alphabetical order with the Card number on which they appear Variable Card Variable Card Variable Card Variable Card AbO3 5a COMNT 1 IOTOT 12b SOLARC 11 AEROS 8 DAY 17a IOUT 12c SPR 2a ALPHA1 8a DSTEP 17a IPRT 12 STEP 14a ALPHA2 8a ELEV 17a ISCAN 14 SUNCOR 11 ALTIT 2a FWHM 14a ISPCTR Ta TAIR 3a AMASS 17a GG 8a ISPR 2 TAU5 9a ApCH20 6b HEIGHT 2a ITILT 10b TAU550 9a ApCH4 6b HOUR 17a ITURB 9 TDAY 3a ApCo 6b IALBDG 10c IUV 16 TILT 10c APERT 13a IALBDX 10 LATIT 2a 17a VISI 9a ApHNO2 6b IALT 5a LIMIT 13a WwW 4a ApHNO3 6b IATMOS 3 LONGIT 17a WAZIM 10c ApNO 6b ICIRC 13 MONTH 17a WLMN 11 ApNO2 6b IFILT 14a OMEGL 8a WLMX 11 ApNO
29. ackward compatible with versions 2 9 and later Consult Section 16 for changes that occurred between versions 2 8 and 2 9 5 New features in this version appear in red CARD 1 COMNT COMNT is a text string that can be any title for the current run or any user s comments on atmospheric conditions etc It is limited to 64 characters max Do not use spaces but rather underscores _ to separate words or character strings if necessary CARD 2 ISPR ISPR is an option for site s pressure ISPR 0 to input SPR on Card 2a ISPR to input SPR ALTIT and HEIGHT on Card 2a ISPR 2 to input LATIT ALTIT and HEIGHT on Card 2a The program calculates ALTIT from SPR assuming HEIGHT 0 if ISPR 0 or calculates SPR from LATIT ALTIT and HEIGHT if ISPR 2 The option ISPR provides more accurate results and is recommended CARD 2a if ISPR 0 SPR SPR Surface pressure mb must be gt 0 0004 mb CARD 2a if ISPR 1 SPR ALTIT HEIGHT SPR Surface pressure mb ALTIT Site s altitude i e elevation of the ground surface above sea level km must be lt 100 km In case of a flying object ALTIT refers to the ground surface below it HEIGHT Height of the simulated object above the ground surface underneath km must be lt 100 km new input The total ALTIT HEIGHT is the altitude of the simulated object above sea level and must be lt 100 km CARD 2a if ISPR 2 LATIT ALTIT HEIGHT
30. angle O to 90 decimal deg i e true astronomical zenith angle MINUS refraction correction AZIM Solar azimuth 0 to 360 decimal deg counted clockwise from North 0 0 toward West 270 0 Note AZIM is only used to calculate radiation on a tilted plane If such calculation is not relevant any value e g 0 0 can be input for this variable CARD 17a if IMASS 1 ELEV AZIM ELEV Solar elevation 0 to 90 decimal deg i e true astronomical elevation PLUS refraction correction AZIM Solar azimuth 0 to 360 decimal deg counted clockwise from North 0 0 toward West 270 0 Note AZIM is only used to calculate radiation on a tilted plane If such calculation is not relevant any value e g 0 0 can be input for this variable CARD I7a if IMASS 2 AMASS AMASS Relative i e non pressure corrected air mass or Rayleigh optical mass must be between 1 0 and 38 2 CARD 17a if IMASS 3 YEAR MONTH DAY HOUR LATIT LONGIT ZONE YEAR A four digit integer e g 2002 MONTH Any integer between 1 and 12 DAY Day of the month 1 31 HOUR Local Standard Time LST in decimal hour CAUTION not to be confused with Local Apparent Time Daylight Saving Time or Universal Time LATIT Site latitude decimal degrees positive North negative South e g 17 533 for Papeete Tahiti LONGIT Site longitude decimal deg Counted positive East of Greenwich negative West of Greenwich e g 104 667 for
31. cutables are provided one for Standard execution and one for Command line or Batch execution They are produced from the same source file just by modifying a single line of code Note to power users See instructions on lines 184 185 of smarts295 f The two executables only differ in the way they are invoked and the way the user is involved during execution See Section 4 for all necessary details 2 1 Standard execution This execution is called standard because it can be started by the usual double click on a script named smarts295 command A shorter filename smarts295 rather appears if the option for displaying extensions is turned off as is the case for the screenshot shown below When this script opens the executable named smarts295_cmd is invoked 2 2 Command line batch execution This execution is commanded by a different executable smarts295bat When it is invoked execution is done transparently and directly without any user intervention using the default input output file names It provides maximum speed of execution 3 HARDWARE AND SOFTWARE REQUIREMENTS Typically any recent MacIntosh computer will produce results in a few tenths of a second to a few seconds depending on case complexity and processing power Daily calculations are extremely processor intensive but results should appear within less than a minute or so This Mac version prefers OSX 10 2 or greater and
32. d options or platform This may therefore lead to varying results from one compiler to the other or one platform to the other So far this problem has been avoided but it is always a good thing to double check that your results are correct This is the role of the solved examples Please report any discrepancy to the author 5 RUNNING THE CODE The only delicate step involved before actually running the code is to prepare a correct input file Careful reading of Section 6 is thus recommended in a first step Then it is advised to start using one of the resolved examples that are provided in the Examples subfolder Their input files are commented for clarity ES IMPORTANT NOTES An incorrect input file will result either in incorrect results or in a runtime error In the latter case the executable will either quit abruptly or engage in an infinite loop that needs to be stopped manually by forcing the application to quit Results are located in one to three output files depending on the desired sophistication The standard output displays only input echo and broadband results in File 16 e g smarts295 out txt Two optional spreadsheet ready output files with spectral results can be requested File 17 e g smarts295 ext txt and File 18 e g smarts295 scn txt File 17 contains spectral results for up to 43 user selectable variables File 18 contains spectral smoothed results for 5 fixed variables Previous user
33. d rather than global horizontal photon flux e Outputs 33 43 are new The trace gases are BrO CH O CINO HNO HNO NH NO NO NO SO The mixed gases are CH CO CO N N O O and O An asterisk indicates a gas that is not considered or only partially considered in MODTRAN4 CARD 13 ICIRC ICIRC is an option controlling the calculation of circumsolar radiation which is useful when simulating any type of radiometer spectral or broadband equipped with a collimator ICIRC 0 bypasses these calculations ICIRC indicates that a typical radiometer needs to be simulated The geometry of its collimator must then defined on Card 13a CARD 13a if ICIRC 1 SLOPE APERT LIMIT SLOPE Slope angle half cone of the simulated radiometer between 0 1 and 10 deg APERT Half aperture or opening angle of the simulated radiometer deg between 0 1 and 10 deg LIMIT Limit angle half cone of the simulated radiometer between 0 1 and 10 deg These half angles fully define the geometry of the simulated radiometer and are bound by the condition SLOPE lt APERT lt LIMIT If SLOPE or LIMIT is set to 0 0 the missing value will be calculated by the program If SLOPE and LIMIT are set to 0 0 the penumbra function will be set to 1 0 an average geometry is thus considered If APERT is unknown it should be set to 0 0 the penumbra function will be calculated transparently from SLOPE and LIMIT only Pr
34. d Fortran code to predict the direct beam diffuse and global irradiance incident on surfaces of any geometry at the Earth s surface It covers the whole shortwave solar spectrum 280 to 4000 nm and thus includes the UVA UVB Visible and Near Infrared bands Besides the regular irradiance predictions needed for many possible applications it can be used to simulate the spectral or broadband irradiance that would be measured by a radiometer such as a spectroradiometer a pyranometer or a pyrheliometer It can also predict the photosynthetically active components of radiation the illuminance on any surface the luminous efficacy of direct diffuse and global radiation the UV index as well as various UV action weighted spectra Version 2 0 of SMARTS was released in 1994 and was described in Gueymard 1994b 1995 A peer reviewed journal paper Gueymard 2001 also gives a partial but updated description of the model current with version 2 8 released November 1996 A separate file History txt details the changes that occurred in the successive versions of the code prior to version 2 9 This User s Manual covers version 2 9 5 which includes considerable improvements over previous versions see Section 14 Background information on the new algorithms and on possible applications of the code in various fields is described elsewhere Gueymard 2005 Gueymard and Kambezidis 2004 Gueymard et al 2002 Myers and Gueymard 2004 The pr
35. e can be treated either as Lambertian L or non Lambertian NL A Lambertian or isotropic surface reflects the incident irradiance equally in all directions Most natural surfaces have a directional reflectance pattern they reflect more in the direction of the solar beam and are thus non Lambertian to some degree The possible values of TALBDX are 1 to input a fixed broadband Lambertian albedo RHOX on Card 10a 0 to read user defined spectral reflectance from file Albedo dat with Lambertian characteristics L 1 if the same dataset from file Albedo dat is to be considered non Lambertian NL 2 if a spectral non Lambertian reflectance for water is to be calculated by the program at run time 3 to 66 if spectral reflectance data are to be read from one of the available 64 default files described below and considered non Lambertian NL New The albedo library has 28 new files in this version they are indicated by a red color in the Table below All reflectance data are read in an appropriate data file except for codes 1 and 2 see above All the possible codes are listed in the table below with the corresponding file names and spectral ranges Note that most spectral ranges are significantly shorter than the maximum range supported by the code If the requested spectral range for the calculations extends beyond the spectral range of an albedo file all missing reflectance values are set equal to the nearest known
36. e input file is constituted of a series of lines representing as many virtual Input Cards Their total number is variable depending on the complexity of the requested calculations If a Card contains inputs for more than one variable they must be separated by a blank space or a coma For clarity commas are used to separate variables in this manual All Card images and their content are described here in their prescribed order of appearance in the input file Variable names and their character value if applicable appear in COURIER bold for easier recognition Quotes around text characters can be omitted e g on Cards 1 3a and 8 There are two types of Cards the Main Cards which are mandatory and should exist in any input file and the Optional Cards whose presence and contents depend on the options selected on the preceding Main Card This is a sample Main Card CARD 3 IATMOS This is a sample Optional Card CARD 3a if IATMOS 1 ATMOS Important discussions about the correct use of variables and data sources of data etc appear in blue type with a red vertical border just like this paragraph Se IMPORTANT NOTES Some input cards and content have been modified since version 2 9 2 They appear in yellow and are marked with a blue star symbol X Existing input files from version 2 9 2 or earlier will not be valid without proper alteration of these input cards Conversely however all 2 9 5 input files are b
37. e turbidity input from Card 9a is ignored 32 2 Receiver is at more than 0 5 km above ground hence the calculation of the reflected irradiance from the ground to the tilted plane is not accurate The albedo specified on Card 10c is for the tilted surface foreground whose area may be relatively small The higher the Receiver is above ground the lesser the effect of this foreground is on the reflected irradiance to the receiver ERROR messages 1 The altitude cannot be gt 100 km RUN ABORTED This corresponds to the assumed outer limit of the atmosphere See Card 2a 2 The value selected or calculated for precipitable water W is which is above the allowed maximum value of 12 cm RUN ABORTED This message is displayed if an incorrect value is entered on Card 4a or if extremely hot and humid conditions are entered on Card 3a 3 Input value for ITURB on Card 9 is gt 5 Please specify a smaller value RUN ABORTED ITURB should be between 0 and 5 See Card 9 4 Input value for turbidity is too large TAU550 Please specify a smaller value RUN ABORTED The maximum allowed value of TAU550 is 5 0 5 Input value for Meteorological Range is lt 1 km Please specify a larger value RUN ABORTED This message is displayed if a too low value is entered on Card 9a The minimum value for RANGE is km and 0 77 km for VISTI 6 Sun is too low for the specified date This condition must be fulfilled Ideclination
38. e water above the site altitude in units of cm or equivalently g cm it must be lt 12 Precipitable water can be determined from radiosonde soundings radiometric methods remote sensing from space or by using GPS positioning delay information In the general case such datasets are not specifically available for the exact desired time and site It is possible to use climatological averages or empirical equations predicting W as a function of surface temperature humidity and pressure See Garrison and Adler 1990 Gueymard 1994a Myers and Maxwell 1992 more specifically for U S or Canadian conditions and many other references for empirical determinations in various other countries W represents the total column of water vapor if condensed in the atmosphere above site level This value is to be input directly if IH20 0 Alternatively it will be calculated by the program from either the user selected reference atmosphere if IH20 1 assuming free atmosphere conditions in this case in reality precipitable water might be higher for an elevated site because of boundary layer effects or from surface data of temperature and humidity if IH20 2 In the latter case the author s empirical model Gueymard 1994a is used The validity of such estimates at high altitude sites including flying objects or at sites outside North America cannot be guaranteed CARD 5 103 IO3 is an option to select the appropriate ozone abundance inp
39. eawater Pacific CSeaWatr NL 0 277 2 976 W 64 Open ocean seawater Atlantic OSeaWatr NLE 0 277 2 976 W 65 Grazing field unfertilized GrazingField NL 0 401 2 499 V 66 Young Norway spruce tree needles Spruce NL 0 39 0 845 V KEY L Lambertian NL Non Lambertian SP Specular M Manmade materials S Soils and rocks U User defined V Vegetation W Water snow or ice The non Lambertian effect is modeled as an increase of reflectance with zenith angle such as Rhob Rhob0 1 cosZ Ln 1 1 cosZ 0 35 Rhod 1 167 Rhob0O for all surfaces except snow codes 3 4 28 and 30 for which the following model is used Rhob Rhob0O 1 0 176 cosZ 0 94 Rhod 0 939 Rhob0O In these equations Rhob is the reflectance for beam radiation Rhod the reflectance for diffuse radiation RhobO the reference reflectance in the data files and cosZ the cosine of the zenith angle ZENIT The measured data are supposed to have been measured at zenith angles of about 20 deg for snow and about 53 deg for all other surfaces including the user defined data in file Albedo dat 19 The spectral reflectance for water code 2 is calculated for each wavelength by the program and uses the Fresnel formula for specular reflectance However codes 35 and 63 64 can be used to select actual measured sea water albedo data along with a non Lambertian rather than specular spatial reflectance distribution CARD 10a if TALBDX 1 RHOX RH
40. ecause often reported in satellite based aerosol datasets for instance See Card 9 A more precise relationship between turbidity and visibility is now used It depends on season and takes into account the presence of tropospheric aerosols above an altitude of 2 km Altitude inputs An additional input variable has been added to describe the vertical position of the object e g aircraft under scrutiny its HEIGHT above ground See Card 2 and other details below Albedo library Twenty eight files have been added to the library see Card 10 The maximum number of lines in each user defined spectral albedo file has been increased to 3000 Irradiance calculations The algorithm used to evaluate diffuse irradiance has been streamlined As a result irradiance predictions appear to be improved compared to spectral measurements particularly in the UV Calculations are now possible for any ground site or to simulate objects instruments whose HEIGHT above sea level is lt 100 km see Card 2 For sites at more than 6 km above sea level turbidity is calculated internally For flying objects the columnar amount of absorbing gases aloft their temperature and other atmospheric variables are extrapolated from ground level defaults if necessary If such values are rather provided by the user they are checked for consistency as a function of altitude Pressure calculations as a function of altitude and latitude have been improved 42 More spectral ou
41. ecise values for these quantities are provided in Table 1 of Gueymard 1998 reproduced below in the case of the most widely used pyrheliometers For instance SLOPE 1 78 deg APERT 2 91 deg and LIMIT 4 03 deg for the Eppley NIP instrument APERT and LIMIT are rarely known for spectroradiometers The precise definition of SLOPE APERT LIMIT is illustrated in the figure below where SLOPE is noted s APERT is noted 4 and LIMIT is noted L Make amp model Slope Opening Limit Eppley NIP 1 78 2 91 4 03 Eppley H F 0 804 23 4 19 Kipp amp Zonen Linke Feussner 1 0 5 08 9 11 Kipp amp Zonen CH1 1 0 2 4 0 Abbott silver disk 0 8 2 9 4 9 24 Detector Fig 1 Geometry of a collimated radiometer CARD 14 ISCAN ISCAN Option for using the scanning smoothing virtual filter of the postprocessor The smoothed results are output on a spreadsheet ready file File 18 smarts295 scn txt This postprocessor is activated if ISCAN 1 not if ISCAN 0 Card 14a is read if ISCAN 1 CARD 14a if ISCAN 1 IFILT WV1 WV2 STEP FWHM IFILT Option for the transmittance shape of the radiometer s optics Select IFILT 0 for a triangular shape IFILT 1 for a Gaussian bell shape WV1 Min wavelength nm to output the smoothed results WV2 Max wavelength nm to output the smoothed results Example WV1 320 5 Wv2 1100 To avoid transitional problems near these limits and
42. ed 1 km deep tropospheric pollution layer ppmv ApSO2 Sulfur dioxide volumetric concentration in the assumed 1 km deep tropospheric pollution layer ppmv SMARTS considers separate gaseous absorption calculations for tropospheric gases typically trapped in a pollution layer This layer is assumed to be 1 km thick above ground and well mixed Default values for the concentration of ten tropospheric gases are transparently used in the program when IGAS 0 and ILOAD 1 4 However selecting IGAS 0 and ILOAD 0 allows the user to provide measured or otherwise estimated concentrations for these 10 gases through variables ApCH20 ApCH4 ApCO ApHNO2 ApHNO3 ApNO ApNO2 ApNO3 ApO3 ApSO2 These concentrations need to be given in ppmv parts per million per volume The program converts these concentrations to equivalent total column abundances on the basis that each gas concentration is constant within the 1 km pollution layer When data of average pollutant concentration are used and the pollution layer is known to be of a different thickness than 1 km the user needs to make a preliminary conversion i e by multiplying the observed average concentration for a H km layer by H 13 To use concentration data provided in atm cm for a H km layer multiply these values by 10 H to obtain the correspondence in ppmv To use concentration data provided in g m multiply these values by 0 022414 M for any H to obtain the correspondence
43. ent possible causes the simplified algorithms used in SMARTS which can affect results in strong absorption bands e g the water vapor bands around 940 nm and 1150 nm the use of more recent or complete absorption data in this version of SMARTS e g for the UV and visible ozone bands and the consideration of more absorbing gases by SMARTS Eight absorbing species now considered in SMARTS are not in MODTRAN yet BrO CH 0 CINO HNO HNO NO O as well as SO in the UV As demonstrated by Fig 4 the dips in the difference curve are attributable to the additional absorption caused by these gases particularly O ASTM G159 Conditions Beam Transmittance Predictions SMARTS vs MODTRAN4 wii E pee tone ene ene SMARTS v 2 9 Transmittance Difference SMARTS2 MODTRAN4 300 400 500 600 700 800 900 1000 1100 1200 1300 Wavelength nm Fig 3 Percent difference between the direct transmittance predicted by SMARTS versions 2 8 and 2 9 and MODTRAN version 4 0 for the same standard conditions 38 Figure 5 shows a comparison between the direct irradiance for an air mass 1 5 and standard atmospheric conditions predicted by SMARTS and the absolute spectral difference in W m nm between the irradiance predictions of SMARTS and MODTRAMN4 For this comparison the Cebula Chance Kurucz spectrum has been used in both codes Finally the data in Fig 5 are shown in greater detail in Fig 6 where the irradiance difference betwee
44. errestrial 896 54 Atmospheric Transmittance 0 6646 FOR THE HORIZONTAL PLANE Direct Beam 597 16 Diffuse 100 13 Global 697 29 Clearness index KT 0 5101 Diffuse irradiance origination details Sky diffuse 87 17 Back scattered diffuse 12 96 FOR THE TILTED PLANE Direct Beam 879 36 Sky Diffuse 124 57 Ground Reflected 23 83 Global 1003 93 EXPERIMENTAL WITH CIRCUMSOLAR CORRECTION Direct Beam Normal Incidence 898 78 Diffuse Horizontal 98 64 Global Horizontal 697 29 51
45. evious official release was version 2 9 2 Versions 2 9 3 and 2 9 4 have only been distributed to a few beta testers As can be understood from Section 16 this new version offers many new features improvements over the previous ones Consequently the spectra predicted with this new version may differ slightly from those obtained with older versions even for the exact same conditions at least over some wavebands Also new to this version is the choice between three platforms Mac OSX Linux and Windows The MacIntosh Classic platform is not supported any more To simplify reading each platform has now separate Manuals this User s Manual and the QuickStart guide Contrarily to previous versions the functionality and purpose of each platform s version is now slightly different The Windows version is aimed at novice users particularly with the use of the graphical User Interface Conversely the Mac OSX and Linux versions are aimed at power users who want to take advantage of the powerful Unix scripting capabilities The core model s features and Fortran code themselves however are strictly the same for all platforms 2 FORTRAN LANGUAGE AND EXECUTABLES Standard Fortran 77 has been used with only a few extensions The source file smarts295 f now contains nearly 6000 lines of code It calls 27 data files during a typical run The executables have been prepared with the open source g77 compiler Two slightly different exe
46. f MODTRAN runs The six default extraterrestrial spectra offered in MODTRAN are now also available in SMARTS for comparative and compatibility purposes However the revised non MODTRAN spectrum described in Section 13 is recommended for normal use 37 Because MODTRAN4 incorporates many changes and improvements over MODTRAN2 on which the previous versions of SMARTS were based it is interesting to compare the predictions of SMARTS versions 2 8 and 2 9 to those of MODTRAMN4 for typical atmospheric conditions Such a comparison is not directly possible because MODTRAN s outputs are in equal steps of wavenumbers with a minimum step of 1 cm rather than wavelengths Thus it has been necessary to resample and degrade MODTRAN s outputs using its maximum resolution to fit SMARTS s own resolution so that wavelength by wavelength correspondence could be achieved The atmospheric conditions were chosen according to ASTM standard E891 87 reissued as standard G159 98 ASTM 1987 1998 and ISO 9845 1 ISO 1992 These same conditions are used in Examples 1 and 3 for the user s benefit Figure 3 shows the percent deviation between the direct atmospheric transmittance predicted by the two versions of SMARTS and by MODTRAN The improvement from version 2 8 to 2 9 is particularly obvious over the whole spectrum A more detailed comparison between SMARTS 2 9 and MODTRAN 4 0 appears in Fig 4 Structure in the difference curve is caused by differ
47. his run Example_6 USSA_AOD 0 084 ATMOSPHERE USSA AEROSOL TYPE S amp F_RURAL INPUTS Pressure mb 1013 250 Ground Altitude km 0 000 Height above ground km 0 000 Relative Humidity 46 040 Precipitable Water cm 1 4160 Ozone atm cm 0 3438 or 343 8 Dobson Units AEROSOLS Optical Depth at 500 nm 0 0840 Optical depth at 550 nm 0 0764 Angstrom s Beta 0 0333 Schuepp s B 0 0365 Meteorological Range km 124 2 Visibility km 95 1 Alphal 0 9640 Alpha2 1 4314 Mean Angstrom s Alpha 1 1977 Season SPRING SUMMER TEMPERATURES Instantaneous at site s altitude 288 1 K Daily average reference at site s altitude 288 1 K Stratospheric Ozone and NO2 effective 225 3 K The following spectral variables will be output to file SMARTS2 EXT Global_tilted_irradiance Beam_normal_ circumsolar Difuse_horiz circumsolar Zonal_ground_reflectance Spectral ZONAL albedo data LIGHT_SANDY_SOIL with a reflection process NON_LAMBERTIAN GEOMETRY half angles OF THE SIMULATED RADIOMETER deg Slope 0 00 Aperture 2 90 Limit 0 00 The radiometer s Slope and Limit angles are not provided Circumsolar calculations will therefore be performed for an average geometry corresponding to the Aperture angle Spectral LOCAL albedo data LIGHT_SANDY_SOIL with a reflection process NON_LAMBERTIAN 50 SOLAR POSITION deg Zenith Angle apparent 48 236 Azimuth from North 180 00 R
48. ic sciences is MODTRAN developed by the Air Force Geophysics Laboratory of Hanscom MA The SMARTS algorithms have been revised in this version to improve the agreement between its predictions and those of MODTRAN version 4 0 Although the algorithms in SMARTS are completely different than those in MODTRAN both codes have some common ground described below 2 The six reference atmospheres used in MODTRAN are part of the library of ten reference atmospheres in SMARTS The different Shettle amp Fenn aerosol models used in MODTRAN are also part of the library of default aerosols in SMARTS Note however that only an approximate fit of the spectral variation of the optical characteristics of these aerosols has been voluntarily used in SMARTS A notable exception has been made for the Rural Aerosol model whose optical depth spectral variations have been closely reproduced with a stepwise regression method Absorption coefficients for some gases have been derived from MODTRAN4 results This is the case for CH CO CO H O NH NO N N O over the whole spectrum and for O and SO in the IR only In all other cases cross section data from the recent spectroscopic literature have been used and temperature correction functions have been considered wherever possible The optical masses for all extinction processes in SMARTS have been fitted to a common equation from slant column abundances obtained by varying the zenith angle in a series o
49. in ppmv where M is the molar mass of the gas in grams Molar masses of the basic species are as follows C 12 H 1 N 14 O 16 S 32 Hence the molar mass of ozone is 48 g and that of NO is 30 g CARD 7 qco2 qCO2 is the carbon dioxide columnar volumetric concentration ppmv The current average CO concentration is about 370 ppmv but fluctuates seasonally and increases over time by about 2 ppmv year It was about 330 ppmv in 1976 hence the default value of 330 ppmv used in the U S Standard Atmosphere Anon 1976 and the LOWTRAN MODTRAN family of atmospheric codes Note that this concentration does not vary appreciably with altitude but does vary slightly with location and date season and year k CARD 7a IsPpcTR ISPCTR is an option to select the proper extraterrestrial spectrum This option allows to choose one out of ten possible spectral files Spctrm_n dat where n 0 8 or n U The following table lists the source for each file and the corresponding solar constant The original data have been resampled and degraded to the best resolution achievable with SMARTS i e 0 5 nm between 280 and 400 nm 1 nm between 400 and 1700 nm and 5 nm between 1705 and 4000 nm Option 0 NEW is for a synthetic spectrum recently proposed Gueymard 2004 and is recommended for normal use Option 1 is for a synthetic spectrum revised from the previous SMARTS 2 8 spectrum which was recommended for use with versions 2
50. ion 2 9 5 Bug correction A bug in all previous versions that affected the calculation of pressure in the southern hemisphere has been corrected Another bug that affected versions 2 9 2 9 1 and early 2 9 2 where a request for more than 24 spectral outputs crashed the program has been corrected Another corrected bug is one that affected all previous versions where incorrect spectral values of direct tilted irradiance were printed on File 17 when a zero tilt horizontal plane was defined The incorrect value that was displayed for the N abundance in the main OUT file has been corrected Finally two bugs affecting the illuminance results in versions 2 9 to 2 9 2 was discovered and corrected The data files VLambda dat and VMLambda dat have been modified accordingly Extraterrestrial spectrum It is now possible to use two new synthetic spectra One is based on the most up to date data Gueymard 2004 and the other one is interpolated from a standard spectrum ASTM 2000 See Card 7a and Section 13 A user defined extraterrestrial spectrum has been added to the available choices but its preparation must follow strict guidelines see Card 7a and Section 8 Aerosol models Two new aerosol models have been added DESERT_MIN for background desert conditions and DESERT_MAX for sand storm conditions see Card 8 Turbidity inputs A new turbidity input option has been added the aerosol optical depth at 550 nm TAU550 It is convenient b
51. is optimized for G4 or G5 processor It has not been tested on older G3 processors nor on future as of this writing Intel based machines 4 SOFTWARE INSTALLATION AND USE The distribution package is compressed After See e098 SMARTS_295_Mac decompression by double clicking on it the f gt z m 48 a SMARTS_295_Mac folder is created SS Se E A Adobe AAgreement_LICENSE txt smarts295 QuickStart_Mac pdf A typical screenshot of the folder is shown inate here The exact appearance depends on your own settings in the Finder Preferences and smarts295bat smarts295 inp txt View options ee All files and subfolders need to be in a unique c A folder which by default is E Z Z SMARTS_295 Mac but can be renamed z z atin The smarts295 inp txt file is a sample input sail SESE file that you can use to familiarize yourself Beg Zw A with the two execution modes described Ls Z Z below z To use a sample input files contained in one oe ia a ab of the subfolders within the Examples folder Ezz Em ZB move the desired smarts295 inp txt file to E E Z the root of the SMARTS_295 Mac folder _ thus replacing any pre existing file of the Gases Soar Source code r same name 14 items 46 49 GB available Z Use an appropriate text editor such as TextEdit TextWrangler or BBEdit to modify the input file smarts295 inp txt according to your needs based on the detailed explanations provided
52. l therefore be performed for an average geometry corresponding to the APERTure angle See Card 13 When the geometry of the collimator tube is not known entirely but its aperture is known which is the most important variable and the most likely to be known circumsolar calculations are performed without significant loss of accuracy 12 Circumsolar calculations cannot be done for this geometry All half angles must be lt 10 deg See Card 13a 13 Ground reflectance data for extend only from to wm whereas the wavelength limits for this run are and wm Consequently reflectance is fixed at below wm and at above pm This message is very frequent It is displayed in nearly all cases where an albedo file is selected rather than a fixed value All these files have been obtained from measurements whose spectral range is relatively limited In particular measurements below 300 nm are 31 nearly impossible due to the weakness of the signal Three files contain data for the full simulation range 280 4000 nm because extrapolation has been used to fill the missing data 8 SOIL 37 DRY SOIL and 38 LITE SOIL Furthermore calculations for IALBDX 2 or IALBDG 2 SEA or LAKE are done for the full spectral range If the simple extrapolation scheme used at run time and described in the message is not appropriate the use of a custom built ALBEDO DAT file is recommended See Card 10 for more details 14 Lower li
53. lations The content of this output file is fixed The OUTPUT to File 17 e g smarts295 ext txt is formatted to create a spreadsheet formatted file the content of which can be tailored to the user s specific needs according to e column 1 Wavelength nm e columns 2 to last i e IOTOT 1 depending on user s choice of 43 possible variables see IOUT on Card 12c Columns of data are separated by a space and have a heading of 24 characters each The OUTPUT to File 18 e g smarts295 scn txt is also formatted to create a spreadsheet formatted file but its content is fixed according to e column 1 WVLGTH Wavelength nm e column 2 ET SPCTRUM Extraterrestrial Irradiance W m e column 3 BEAM NORM True Direct Beam Irradiance at Normal Incidence W m e column 4 BEAM_NORM Experimental Beam Irradiance at Normal Incidence W m e column 5 GLOB_HORIZ Global Horizontal Irradiance W m column 6 GLOBL_TILT Global Tilted Irradiance W m Columns of data are separated by a space A two line header recapitulates the instrumental characteristics selected Output files 17 and 18 can be read directly in TEXT format by a spreadsheet program such as Microsoft Excel or by plotting software such as Synergy s Kaleidagraph Select a space separator in the Open or Import window if format recognition is not automatic 10 TROUBLESHOOTING WARNING amp ERROR MESSAGES If the code crashes d
54. mit for scans needs to be gt WV1 0 5 FWHM This is in fact a non fatal error more than a warning specifying a too large spectral range for the scan bypasses the smoothing post processor but all other calculations and results are not affected See Card 14a 15 Lower limit for scans is not gt WV1 FWHM This will reduce accuracy in the results for the first wavelengths The post processor can operate but the accuracy at the shorter wavelengths is not guaranteed See Card 14a 16 Upper limit for scans needs to be lt WV2 0 5 FWHM Symmetrical to message 14 above 17 Upper limit for scans is not lt WV2 FWHM This will reduce accuracy in the results for the last wavelengths Symmetrical to message 15 above 18 Parameter INTVL on Card 12a is too low and will be defaulted to 0 5 nm Spectral outputs cannot be reported at a spectral step less than the calculation step 19 Error in albedo file Number of data rows is but should be lt 3000 High resolution albedo data files cannot be used This test prevents the inadvertent corruption of data files from the library and the construction of a too long ALBEDO DAT file by the user See Section 8 20 Receiver is at more than 6 km above sea level hence the aerosol optical depth has been fixed to a default value dependent only on altitude Whenever the elevation above sea level z is more than 6 km TAU550 is calculated from TAU550 exp 3 2755 0 15078 z and th
55. n the predictions of the Monte Carlo BRITE code that was originally used to develop the spectra in standards ASTM G159 and ISO 9845 1 and those of MODTRAN is added for comparative purposes It can be concluded that the gain in accuracy between BRITE and SMARTS is about an order of magnitude at least for these particular conditions ASTM G159 Conditions Beam Transmittance SMARTS 2 9 vs MODTRAN 4 0 2 Uncertainty Band SMARTS2 MODTRANG 300 400 500 600 700 800 900 1000 1100 1200 1300 Wavelength nm Fig 4 Percent difference between the direct transmittance predicted by SMARTS 2 9 and MODTRAN 4 0 showing the additional absorption bands indicated by arrows and the corresponding gases considered in SMARTS 39 1 2 ASTM G159 Atmospheric Conditions Beam Irradiance Predictions SMARTS v 2 9 vs MODTRAN v 4 1 0 E 08 E z 8 0 6 ko 8 04 0 2 ep gt JI n 0 04 O z 0 02 J gt 0 Z 0 02 3 0 04 3 300 500 700 900 1100 1300 1500 1700 Wavelength nm Fig 5 Direct irradiance at normal incidence predicted by SMARTS top panel and its absolute difference with that predicted by MODTRAN 4 0 bottom panel for the same standard conditions 40 ho Atmospheric Conditions of ASTM G159 Dierct Normal Irradiance predictions SMARTS 2 9 and BRITE G159 vs MODTRAN 4 0 0 0 Z SMARTS 2 9 MODTRAN 4 0 e BRITE G159 MODTRAN 4 0 Absolute Difference
56. oes not stop properly or only provides an echo of the input it is highly probable that the input file has not been prepared correctly A missing line a missing input on a line an unphysical or unreadable input value or a misplaced line are typical culprits Double checking the input file is the best way to correct the problem 29 A run time error happens any time the output files that have been created in a previous run are still in the same directory and have not been renamed Deleting or renaming them will simply solve the problem More subtle problems may surface if the numerical values of some inputs are not appropriate In the most minor cases the code will run anyway but will output WARNING messages to signal the problem and possibly inform the user of any interpretation or extrapolation it had to do In more severe cases an ERROR message is issued and the run is aborted Most of these messages are relatively self explanatory but they are all listed and discussed below for further reference WARNING messages 1 The calculated ozone temperature was below the most probable minimum of for this altitude The latter value has been used for optimum results Suggestion double check the daily temperature on input Card 3a The effective ozone temperature is now calculated from the daily average temperature at the altitude of the simulated receiver A good estimate of the latter is therefore necessary 2 The calculated ozone tem
57. olumn above an object flying at more than 2 km above ground is always forced to respond to the tropospheric model 8 The aerosol optical depth at 550 nm is outside the most probable limits of and for this altitude assuming a slight background amount of volcanic aerosols This may produce inconsistent results Suggestion double check the value of your turbidity input on Card 9a This message is generated if the geometric altitude of the simulated object above sea level i e HEIGHT ALTIT is between 15 and 22 km where more volcanic aerosols than normal background may exist In practice it may be difficult to estimate the aerosol abundance above a high flying object The typical minimum and maximum limits provided in this message may be used as a guideline 9 The aerosol optical depth at 550 nm is outside the most probable limits of and for this altitude This may produce inconsistent results Suggestion double check the value of your turbidity input on Card 9a Same as message 8 just above but for altitudes below 15 km or above 22 km No volcanic aerosol is normally present at these altitudes 10 The values of both APERT and SLOPE or LIMIT for the circumsolar correction are incorrectly less than or equal to 0 This calculation is therefore skipped The collimator s geometry must be better defined See Card 13 11 The radiometer s SLOPE and LIMIT angles are not provided Circumsolar calculations wil
58. onding solar constant which is read by the program For each wavelength the program then multiplies the extraterrestrial irradiance by the scaling factor described above This scaling process is identical to what is done in MODTRAN 4 0 See ISPCTR Card 7a for a description of each of the eight spectrum files CARD 12 IPRT IPRT is an option to select the results to be printed on Files 16 and 17 Only broadband results are output to File 16 if IPRT 0 Spectral results are added to File 16 and Card 12a is read if IPRT 1 Spectral results are rather printed to File 17 in a spreadsheet like format if IPRT 2 Finally spectral results are printed to both File 16 and 17 if IPRT 3 Cards 12b and 12c are read if IPRT 2 or 3 see IOTOT and IOUT Note that the spectral results printed on File 16 with IPRT 1 are limited in scope to the direct diffuse and global irradiances For improved control and a larger choice of printable variables use IPRT 2 or 3 Note also that the spectral results of the smoothing postprocessor Card 14 are printed on another spreadsheet ready file File 18 irrespective of IPRT CARD 12a Gf IPRT gt 1 WPMN WPMX INTVL WPMN WPMX Spectral range or min and max wavelengths nm between which results will be printed on File 16 SMARTS295_OUT txt and or File 17 smarts295 ext txt if IPRT 1 to 3 on Card 12 These conditions must be respected WPMN gt WLMN WPMX lt WLMX Example WPM
59. orresponds to the zonal albedo large scale e g 10 100 km used in backscattering calculations RHOG rather corresponds to the local albedo small scale e g 1 1000 m required when converting irradiance incident on a horizontal plane to that incident on a tilted plane RHOG is then the broadband reflectance of the horizontal foreground immediately in front of the tilted receiver itself assumed of small dimensions e g a solar collector a window In general RHOG and RHOX have different values because the ground surface is rarely uniform over large areas However the value of RHOX can be used for RHOG if the tilted receiver has a nearly infinite area e g a mountain slope Note also that RHOG and RHOX are both broadband average albedo values i e spectrally fixed reflectances Such a case is almost never found in nature so that calculations based on these values will be simplistic For more realistic spectral calculations use the library of 64 spectral reflectance files for natural surfaces all obtained from spectral measurements see TALBDG and IALBDX or use site specific spectral albedo values with the user defined Albedo dat file 20 CARD 11 WLMN WLMX SUNCOR SOLARC WLMN WLMX Spectral range in nm or min and max wavelengths between which all spectral calculations will be performed WLMN should be 280 0 nm and WLMX should be lt 4000 nm e g WLMN 300 5 WLMX 1810 SUNCOR is a correction fac
60. p ERROR MESSAGES sssesesseseosessoscseosessoscseoscseososeoroseososeseosessoseseoecseeeosesees 29 11 SAMPLE RUNS AND PRINTOUT ccsssssssssssscscsssssssscsssessssssssessssesssessssssesesessssesasessssssssessssseesacessssesacessssssacessssees 34 12 UV ACTION WEIGHTED IRRADIANCE G cccssssssssssscssssssssssssessssesssesssscsssacessssscasessssssssessessessessssssesacessssessesesseess 34 13 REVISED EXTRATERRESTRIAL SPECTRUM csssssssssssssssscsssesssscsesssssssscsssessssssssessssssasessssssasesssssesesssessees 35 14 COMPARISONS WITH MODTRAN cccsssssssscsssssssscscsssssssscsssesssscsssessssssesesessesssasessssssasessesssssssensssasscsessseseesssseass 37 15 APPLICATIONS scssssssssscsssssssossscssssscsssessssesssesssscssssssssssassssscsssacsssssssacessssssassssssssasassssssssacesssoussssssssssssssessassssssssars 41 16 SUMMARY OF NEW FEATURES IN VERSION 2 9 X cccssssssssssscsssessssosesesessssssasessesssssesessesesssessesesacessesesacessesees 42 17 REFERENCE G ccssssssssssssosesssssoscssssssssssasessssssessssssssssasesssssassssssssssesssscsssacsssssssassssssssacessesssasessssssasacossssosacsssssssasessssees 46 Solar Consulting Services 2005 2006 ulting Please report any problem or success stories to the author rvices Email address Chris SolarConsultingServices com 1 INTRODUCTION SMARTS Simple Model of the Atmospheric Radiative Transfer of Sunshine is a spectral model an
61. perature was above the most probable maximum of for this altitude The latter value has been used for optimum results Suggestion double check the daily temperature on input Card 3a Symmetrical to 1 just above 3 The ozone columnar amount atm cm is outside the most probable limits of and for this altitude This may produce inconsistent results Suggestion double check the values of IALT and AbO3 on input Card Sa Consistency between IALT and AbO3 is important particularly for a high flying object In such a case either the ground value of AbO3 is used and IALT set to I or the local value of AbO3 is used and IALT set to 0 See Card 5a for discussion 4 Pressure cannot be lt 0 00041 mb and has been increased to this value See Card 2 5 Precipitable water was not provided and no reference atmosphere was specified USSA conditions have been used here See Card 4 6 The ozone amount was not provided and no reference atmosphere was specified USSA conditions have been used here See Card 5 30 7 The aerosol type has been changed to S amp F_TROPO because the height above ground is gt 2 km Only the aerosols in the well mixed layer assumed to have a fixed thickness of 2 km independent from the ground altitude above sea level are allowed to have very variable physical and optical characteristics Above this layer all aerosols are considered obeying to the tropospheric model Hence the aerosol c
62. pl Opt 34 2765 2773 Caldwell M M 1971 Solar UV irradiation and the growth and development of higher plants in Photophysiology A C Giese ed vol 6 Academic Press p 131 177 Caldwell M M et al 1986 Action spectra and their role in assessing biological consequences of solar UV B radiation change in Stratospheric ozone reduction solar ultraviolet radiation and plant life R C Worrest and M M Caldwell eds Springer Verlag Berlin p 87 111 Coblentz W W and Stair R 1934 Data on the spectral erythemic reaction of the untanned human skin to ultraviolet radiation U S Bur Stand J Res 12 13 14 De Fabo E C Noonan F P and Frederick J E 1990 Biologically effective doses of sunlight for immune suppression at various latitudes and their relationship to changes in stratospheric ozone Photochem Photobiol 52 811 817 de Gruijl F R and Van der Leun J C 1994 Estimate of the wavelength dependency of ultraviolet carcinogenesis in humans and its relevance to the risk assessment of a stratospheric ozone depletion Health Phys 67 319 325 Diffey B L 1982 The consistency of studies of ultraviolet erythema in normal human skin Phys Med Biol 27 715 720 Garrison J D and Adler G P 1990 Estimation of precipitable water over the United States for application to the division of solar radiation into its direct and diffuse components Solar Energy 44 225 241 Green A E S and Mo T 1974 An epidemiological
63. problems it is recommended to move the output files to the OUTPUT folder or any other folder before the next run 5 4 3 Advanced scripts for batch processing Unix offers a series of shell commands that can enhance the batch capabilities of the SMARTS code A sample shell file called smarts295script csh is provided in the Source_code folder It makes use of the smarts295bat executable see previous paragraphs The content of this file is listed below A user familiar with shell scripting can take further advantage of the batch mode and create even more complicated scripts bin csh Use source smarts295script csh to execute this file or chmod u x smarts295script csh and then smarts295script csh foreach i 01 02 03 04 june july 20050914 cp f smarts Si inp txt smarts295 inp txt smarts295bat mv smarts295 out txt smarts i out txt mv smarts295 scn txt smarts i scn txt mv smarts295 ext txt smarts i ext txt end This example script assumes that seven input files are present in the root folder with a variety of naming conventions for demonstration purposes smarts_Ol inp txt smarts_02 inp txt smarts_O3 inp txt smarts_04 inp txt smarts_june inp txt smarts_july inp txt and smarts_20050914 inp txt When the script is activated after it is moved to the root of the main folder and the instructions from the comments in the first few lines of the script are
64. re to be defaulted using average vertical profiles CARD 6a if IGAS 0 ILOAD ILOAD is an option for tropospheric pollution only used if IGAS 0 For ILOAD 0 Card 6b will be read with the concentrations of 10 pollutants ILOAD selects default PRISTINE ATMOSPHERIC conditions leading to slightly reduced abundances of some gases compared to the initial default obtained with the selected reference atmosphere Setting ILOAD to 2 4 will increase the concentration of the 10 pollutants to possibly represent typical urban conditions LIGHT POLLUTION ILOAD 2 MODERATE POLLUTION ILOAD 3 and SEVERE POLLUTION ILOAD 4 Note that these additional gas loads may not all correspond to realistic conditions because each site is different and pollution conditions change rapidly over time Thus it may well happen that for a specific site and time some gases are in reality more abundant than what the default proposes whereas other gases are less abundant These loads must therefore only be considered as subjective guidelines If measured data are accessible the option ILOAD 0 is preferable The following table indicates the defaulted additional tropospheric concentrations in ppmv for each pollutant The number within brackets indicates the value of ILOAD Note that in the case of CH O CO HNO NO and O their ground level concentration under a Pristine Atmosphere is lower than that for the standard conditions of the reference
65. s are now available with all the related input output files and a description in a ReadMe file This User s Manual 45 17 REFERENCES ACGIH 1978 Threshold limit values for chemical substances and physical agents in the workshop environment with intended changes for 1978 American Conference of Governmental Industrial Hygienists Anon 1976 U S Standard Atmosphere 1976 NOAA NASA USAF Washington DC ASTM 1987 Standard tables for terrestrial direct normal solar spectral irradiance for air mass 1 5 Standard E891 87 American Society for Testing and Materials Philadelphia PA ASTM 1998 Standard tables for references solar spectral irradiance at air mass 1 5 Direct normal and hemispherical for a 37 tilted surface Standard G159 98 American Society for Testing and Materials West Conshohocken PA ASTM 2000 Standard solar constant and zero air mass solar spectral irradiance tables Standard E490 00 American Society for Testing and Materials West Conshohocken PA Bj rn L O 1989 Computer programs for estimating ultraviolet radiation in daylight in Radiation measurement in photobiology B L Diffey ed Academic Press p 161 189 Blanco Muriel M et al 2001 Computing the solar vector Solar Energy 70 431 441 Bodhaine B A et al 1999 On Rayleigh optical depth calculations J Atmos Ocean Technol 16 1854 1861 Bucholtz A 1995 Rayleigh scattering calculations for the terrestrial atmosphere Ap
66. s will notice a major overhaul in the file naming conventions This is to streamline the use of extensions accelerate filename typing in command lines and avoid coexistence problems if an older version e g 2 9 2 needs to be used concurrently Each of the sample runs resides in a single Example folder subdirectory with corresponding comments in a ReadMe file These sample runs can be extremely valuable to get accustomed to the code and preview its capabilities In any case it is important to become familiar with the different variables that constitute the input file This is the goal of the next Section Once the input file is ready e g smarts295 inp txt or Test_for_July inp txt and correctly located in the main folder directory the program can be launched using the various alternative methods described in the previous Section k IMPORTANT NOTE The program will NOT execute if any output file eg smarts295 out txt smarts295 ext txt or smarts295 scn txt already exists in this folder An error message would result as described in Section 4 1 It is thus important to RENAME the output files before proceeding to a new run or to move them to a different folder 6 INPUT PREPARATION All inputs are contained in file smarts295 inp txt but as mentioned above it can be renamed to filename inp txt where filename stands for any user defined name e g Test_for_July Th
67. st in different photobiological applications Fourteen such action weighted irradiances are calculated by the program as detailed below e Erythemal irradiance according to five different studies The most widely used erythema spectrum is that of McKinley and Diffey 1987 also known as the CIE erythema spectrum Separate results using older erythema spectra are also reported by the program for comparative purposes These include the fit proposed by Green and Mo 1975 from the original data of Coblentz and Stair 1934 the Diffey erythema spectrum Diffey 1982 modified by Bj rn 1989 the equation of Green et al 1974 derived from the data of Komhyr and Machta 1973 and the equation of Bj rn 1989 obtained by fitting the data of Parrish et al 1982 e The biological action curve of Caldwell 1971 as fitted by Green et al 1974 e The ACGIH safety spectrum ACGIH 1978 as fitted by Wester 1981 1984 e The photosynthesis inhibition spectrum and the polychromatic action spectrum for higher plants according to Caldwell et al 1986 The plant DNA spectrum fit of Green and Mo 1975 from data of Setlow 1974 e The systematic immunosuppression spectrum of De Fabo et al 1990 e The skin carcinogenesis spectra fro humans and mice of de Gruijl and Van der Leun 1994 The spectrum for DNA to protein crosslinks by Peak and Peak 1982 The three latter datasets have been fitted to manageable functions by
68. t shown Irradiance Comparisons Percent Difference SMARTS 2 9 ASTM E490 00 Kurucz 280 300 320 340 360 380 400 Wavelength nm Fig 2a Wavelength by wavelength irradiance difference between some existing spectra and the new default spectrum of SMARTS in the UV region 35 10 Irradiance Comparisons with Synthetic Spectrum Percent Difference SMARTS 2 9 ASTM E490 00 Kurucz 400 450 500 550 600 650 700 Wavelength nm Fig 2b Wavelength by wavelength irradiance difference between some existing spectra and the new default spectrum of SMARTS in the visible region Irradiance Comparisons with Synthetic Spectrum Percent Difference SMARTS 2 9 ASTM E490 00 Kurucz 700 750 800 850 900 950 1000 1050 1100 Wavelength nm Fig 2c Wavelength by wavelength irradiance difference between some existing spectra and the new default spectrum of SMARTS in the near IR region from 700 to 1100 nm 36 Percent Difference Irradiance Comparisons with Synthetic Spectrum SMARTS 2 9 ASTM E490 00 Kurucz 1100 1200 1300 1400 1500 1600 1700 Wavelength nm Fig 2d Wavelength by wavelength irradiance difference between some existing spectra and the new default spectrum of SMARTS in the near IR region from 1100 to 1700 nm 14 COMPARISONS WITH MODTRAN It would be difficult to argue against the statement that the currently pre eminent if not de facto standard radiative transfer code in atmospher
69. th circumsolar Experimental diffuse horizontal irradiance Circumsolar irradiance within radiometer field of view Global tilted photon flux per wavelength Direct normal photon flux per wavelength Diffuse horizontal photon flux per wavelength Rayleigh transmittance Ozone transmittance Transmittance from all trace gases Water vapor transmittance Mixed gas transmittance Aerosol transmittance Beam radiation transmittance Rayleigh optical thickness Ozone optical thickness Optical thickness from all trace gases Water vapor optical thickness Mixed gas optical thickness Aerosol optical thickness Aerosol single scattering albedo Aerosol asymmetry factor Zonal surface reflectance Local ground reflectance Atmospheric reflectance Global foreground reflected irradiance on tilted surface Upward hemispheric ground reflected irradiance Global horizontal photosynthetic photon flux Direct normal photosynthetic photon flux Diffuse horizontal photosynthetic photon flux Global tilted photosynthetic photon flux Spectral photonic energy Global horizontal photon flux per eV Direct normal photon flux per eV Diffuse horizontal photon flux per eV Global tilted photon flux per eV New or modified for 12 in this version 23 Unit HZ ZEEE EEE BEB BRS BBS S SE Wm Wm pmol m s nm pmol m s nm umol m s nm pmol m s nm eV 1 1 1 1 Changes in this version are e Output 12 is now for global tilte
70. the main simulation limits defined on Card 11 the following rules must be followed WV1 gt WLMN FWHM WV2 lt WLMX FWHM WV2 WV1 gt 2 FWHM 25 STEP Interval nm at which the smoothed irradiance results will be printed e g STEP 2 5 FWHM Full Width at Half Maximum i e characteristic bandwidth of the filter transmittance or radiometer spectral response chosen to smooth the output spectral data e g FWHM 6 15 CARD 15 ILLUM ILLUM Option for illuminance luminous efficacy and photosynthetically active radiation PAR calculations These calculations take place if ILLUM 1 1 2 or 2 and are bypassed if ILLUM 0 With ILLUM 1 or 1 illuminance calculations are based on the CIE photopic curve or Vlambda curve of 1924 as supplied in File VLambda dat With ILLUM 2 or 2 the same calculations are done but the revised CIE photopic curve of 1988 is rather used from File VMLambda dat Note that selecting ILLUM 1 or 1 will override WLMN and WLMX see Card 11 so that calculations are done between at least 360 and 830 nm Moreover if ILLUM or 2 luminous efficacy calculations are added to the illuminance calculations This overrides the values of WLMN and WLMX on Card 11 and replaces them by 280 and 4000 respectively New Broadband PAR calculations are performed whenever ILLUM 0 Spectral PAR calculations are always performed see outputs corresponding to IOUT 35 38 on Card 12c
71. tor equal to the inverse squared actual radius vector or true Sun Earth distance e g SUNCOR 1 024 SUNCOR varies naturally between 0 966 and 1 034 adding 3 4 to the irradiance in January and reducing it by 3 4 in July It is calculated by the program if the solar position is calculated from date amp time i e if IMASS 3 on Card 17 thus overwriting the input SUNCOR value on Card 11 If solar position is directly input instead IMASS 3 SUNCOR should be set to 1 0 if the average extraterrestrial irradiance or solar constant see SOLARC is to be used or to any other number between 0 966 and 1 034 to correct it for distance if so desired SOLARC is the selected Solar constant W m The current ASTM standard value is 1366 1 W m and the WMO accepted value is 1367 W m At runtime all spectral irradiances are uniformly multiplied by a constant scaling factor equal to SOLARC divided by the total extraterrestrial irradiance corresponding to the selected spectrum This one is chosen among the eight possible data files Spctrm_n dat with ISPCTR Card 7a These eight files contain the best current estimates of the extraterrestrial spectrum in the 280 4000 nm spectral range For each of these files the solar constant is slightly larger than the integrated irradiance from 280 to 4000 nm because it also includes the contributions for wavelengths below 280 nm and above 4000 nm The second line of each file indicates the corresp
72. tovoltaic applications Annual Meeting of SPIE Denver CO 2004 47 Myers D R and Maxwell E L 1992 Hourly estimates of precipitable water for solar radiation models Proc Solar 92 Cocoa Beach FL Amer Solar Energy Soc pp 317 322 Parrish J A Jaenicke K F and Anderson R R 1982 Erythema and melanogenesis action spectra of normal human skin Photochem Photobiol 36 187 191 Peak M J and Peak J G 1982 Single strand breaks induced in Bacillus subtilis DNA by ultraviolet light action spectrum and properties Photochem Photobiol 35 675 680 Setlow R B 1974 The wavelengths in sunlight effective in producing skin cancer a theoretical analysis Proc Nat Acad Sci USA 71 3363 3366 Shettle E P and Fenn R W 1979 Models for the aerosols of the lower atmosphere and the effects of humidity variations on their optical properties Rep AFGL TR 79 0214 Air Force Geophysics Lab Hanscom MA Van Heuklon T K 1979 Estimating atmospheric ozone for solar radiation models Solar Energy 22 63 68 Wester U 1981 A simple formulae approximation of the ACGIH curve of relative spectral effectiveness of actinic UV Int Rep RI 1981 02 Dept of Radiation Physics Karolinska Inst Sweden Wester U 1984 Solar ultraviolet radiation in Stockholn Examples of spectral measurements and influences of measurement error parameters Int Rep RI 1984 03 Dept of Radiation Physics Karolinska Inst Sweden 48 APPENDIX
73. tput file filename OUT and correspond exactly to the spectral values reported on the optional output file filename EXT Finally the output details for Day of Month and Day of Year are now correctly reported for both Local Time and Universal Time e Turbidity inputs An improved relationship between turbidity and meteorological range is now used for better correspondence with MODTRAN results It is season dependent and takes the influence of tropospheric aerosols above the boundary layer into account The aerosol optical depth at 550 nm is now calculated and printed in the input echo section of filename OUT This wavelength corresponds to the peak of the photopic curve and is the effective wavelength used when deriving the aerosol optical depth from the meteorological range Version 2 9 1 Bug correction A bug in version 2 9 affected calculations with all reference atmospheres except USSA It prevented the correct value of the default precipitable water to be used so that the USSA value was rather used in all cases if IH20 1 was selected on Card 4 e Output variables The number of spectral variables is no more limited to 24 by IOTOT on Card 12b All 32 variables can now be printed on File 17 filename EXT e Scanning smoothing output Results of the scanning smoothing routine if ISCAN 1 on Card 14 are now printed on a separate spreadsheet ready output file File 18 filename SCN for more flexibili
74. tput options are possible see Card 12c In particular various components of photon fluxes and photosynthetic active radiation PAR are now calculated Optionally broadband PAR energy flux and quantum flux can also be output see Card 15 More tests are done on the input data to avoid unphysical situations The existing Warning and Error messages have been streamlined and more have been added see Section 10 Two new sets of sample calculations Examples 10 and 11 have been added e File management File naming has been streamlined with all input and output files now having a txt extension All extraterrestrial spectra are now in the Solar folder all absorption data files are in the Gases folder all albedo data files are in the Albedo folder and all examples including two new examples are in the Examples folder The user interaction during execution as well as the method to invoke the executables have also been streamlined Version 2 9 2 Bug correction A bug in version 2 9 1 that affected calculations with one albedo file IALBDX and IALBDG 2 has been corrected Another fix was a bug that potentially affected all previous versions and was causing numerical instability when calculating irradiances at large air masses The spectral optical depths for water vapor and other gases are now correctly reported when more than one sub run solar position is requested The aerosol optical depths are now correctly reported on the main ou
75. ty 43 Main output file Labelling and content of the main output file File 16 filename OUT has been slightly revamped for clarity Version 2 9 New algorithm for the sun position The authors of the new algorithm Blanco Muriel et al 2001 claim that it is more accurate than Michalsky s algorithm that was used in previous versions Month and Day of month are now used as inputs rather than day of year which might be easier Local Apparent Time LAT is now an output of the program The time zone sign convention has been reversed to become consistent with the longitude sign convention e Improved resolution Resolution has been doubled in the UV below 400 nm 0 5 nm rather than 1 nm The total number of wavelengths is now 2002 from 280 to 4000 nm e Revised extraterrestrial solar spectrum The new spectrum corresponds more closely to the currently accepted solar constant 1367 W m Additionally there are 6 optional spectra from as many possible default spectra in MODTRAN4 Wehrli WRC WMO oldkur newkur chkur cebchkur and thkur These datasets have been resampled and degraded from their original resolution 1 cm to that of SMARTS to accommodate the latter s resolution As in MODTRAN these spectral irradiances can now be scaled to 1367 W m or any other solar constant value if so desired e Revised Rayleigh scattering function The coefficients in the Rayleigh optical depth formulation Tr P Po a
76. ust have created two separate output files smarts295 out txt and smarts295 ext txt both located at the root of the SMARTS_295 Mac folder e If you rather type n or no and hit Enter the following message appears SMARTS 295 gt What is the path to the input file Type only if in the same folder Do NOT type the last of the chain 2000 characters max gt 6 99 Type the path and filename of the input file you want to use or type if the file resides in the current folder For instance type INPUT if it is located in the INPUT folder of SMARTS_295_Mac or type something like SMARTS _inputs Solar First_tests in the case of nested folders elsewhere etc Hit Enter and the program will ask for the proper filename SMARTS 295 gt Generic name for all input output files without any extension 100 characters max gt For instance type Test_for July if the input file is Test_for_July inp txt Hitting Enter results in SMARTS 295 gt You chose the following filenames Input INPUT Test_for July inp txt Output INPUT Test_for July out txt Spreadsheet ready INPUT Test_ for July ext txt Smoothed results INPUT Test_for July scn txt SMARTS 295 gt Is this OK Y N gt Type y if it is OK or n if not and hit Enter If you choose yes execution starts normally and finishes identically as before If you choose to reply
77. ut I03 0 to input IALT and AbO3 on Card 5a I03 1 to use a default value for AbO3 according to the reference atmosphere selected by IATMOS If IATMOS 1 USSA will be defaulted for this calculation if I03 0 IALT AbO3 IALT is an option to select the appropriate ozone column altitude correction IALT 0 bypasses the altitude correction so that the value of AbO3 on Card 5a is used as is IALT should be rather used if a vertical profile correction needs to be applied in case of an elevated site when the value of AbO3 is known only at sea level This option is useful for instance when using ozone data from a ground based instrument located at sea level to estimate the ozone abundance at a distant and elevated site e g on top of an island mountain or in the case of a flying object HEIGHT gt 0 AbO3 site level if IALT 0 or sea level if IALT 1 ozone total column abundance normally excluding tropospheric pollution atm cm The normal range for AbO3 is 0 2 to 0 5 atm cm The present record lows over Antartica are just below 0 1 atm cm The range for the 10 reference atmospheres is 0 28 to 0 38 with an average of 0 3341 close to USSA s value 0 34379 atm cm Van Heuklon 1979 proposed an equation to obtain the average ozone column as a function of latitude longitude and day of the year A better alternative is to use measured data either from satellite based sensors such as TOMS http jwocky gsfc nasa gov
78. value at run time 17 Code Description File name Reflection Spectral Category DAT extension _type range um 1 Fixed broadband albedo L 0 28 4 0 U O User defined spectral reflectance Albedo L User U defined 1 User defined spectral reflectance Albedo NL User U defined 2 Water or calm ocean calculated SP 0 28 4 0 W 3 Fresh dry snow Snow NL 0 3 2 48 W 4 Snow on a mountain neve Neve NL 0 45 1 65 W 5 Basalt rock Basalt NL 0 3 2 48 S 6 Dry sand Dry_sand NL 0 32 0 99 S 7 Sand from White Sands NM WiteSand NL 0 5 2 48 S 8 Bare soil Soil NL 0 28 4 0 S 9 Dry clay soil Dry_clay NL 0 5 2 48 S 10 Wet clay soil Wet_clay NL 0 5 2 48 S 11 Alfalfa Alfalfa NL 0 3 0 8 V 12 Green grass Grass NL 0 3 1 19 V 13 Perennial rye grass RyeGrass NL 0 44 2 28 V 14 Alpine meadow Meadow1 NL 0 4 0 85 V 15 Lush meadow Meadow2 NL 0 4 0 9 V 16 Wheat crop Wheat NL 0 42 2 26 V 17 Ponderosa pine tree PineTree NL 0 34 2 48 V 18 Concrete slab Concrete NL 0 3 1 3 M 19 Black loam BlckLoam NL 0 4 4 0 S 20 Brown loam BrwnLoam NL 0 4 4 0 S 21 Brown sand BrwnSand NL 0 4 4 0 S 22 Conifer trees Conifers NL 0 302 4 0 V 23 Dark loam DarkLoam NL 0 46 4 0 S 24 Dark sand DarkSand NL 0 4 4 0 S 25 Decidous trees Decidous NL 0 302 4 0 Yy 26 Dry grass sod DryGrass NL 0 38 4 0 V 27 Dune sand DuneSand NL 0 4 4 0 S 28 Fresh fine snow FineSnow NL 0 3 4 0 W 29 Green rye grass sod GrnGrass NL 0 302 4 0 V 30 Granular snow GrnlSnow NL 0 3 4 0 W 3l Light clay LiteClay NL
79. ve levels pristine conditions light pollution moderate pollution and severe pollution Variable CO concentration Like in MODTRAN the atmospheric CO concentration which is slowly increasing over time is a user input Revised relationship between visibility and aerosol optical depth It is now based on MODTRANS results Improved fits for Angstr m s wavelength exponent More accurate fits of f wavelength humidity have been obtained for Shettle amp Fenn s aerosol models Improved albedo library The number of albedo data files has been doubled now incorporating some wide range spectral datasets from JPL s ASTER Spectral Library Version 1 2 available on line or on CD ROM from the Jet Propulsion Laboratory http speclib jpl nasa gov More accurate smoothing Improved accuracy and functionality for the SCAN smoothing postprocessor have been implemented It has a better tail rejection for wavelengths away from the peak wavelength and can now cover the whole spectrum in one pass Daily run A daily run can now be specified to calculate the mean daily broadband irradiation in MJ m for any month at a specified location UV Index The UV Index is now reported when requesting the optional extra UV calculations Faster batch runs A simpler interface is used to expedite batch runs Corrections A few bugs that have been reported by users of version 2 8 have been corrected Examples Nine documented Example
80. y applications of a versatile spectral solar irradiance model A review Energy 30 1551 1576 Gueymard C and Kambezidis H 2004 Solar spectral radiation in Solar Radiation and Daylight Models T Muneer ed Elsevier Amsterdam Gueymard C Myers D and Emery K 2002 Proposed reference irradiance spectra for solar energy systems testing Solar Energy 73 443 467 IAMAP 1986 A preliminary cloudless standard atmosphere for radiation computation Rep WCP 112 WMO TD No 24 World Meteorological Organization ISO 1992 Solar energy Reference solar spectral irradiance at the ground at different receiving conditions Part 1 Direct normal and hemispherical solar irradiance for air mass 1 5 Standard ISO 9845 1 International Organization for Standardization Geneva Koepke P et al 1998 Comparison of models for UV index calculations Photochem Photobiol 67 657 662 Komhyr W D and Machta L 1973 in The perturbed troposphere of 1990 and 2020 CIAP vol 4 Dept of Transportation Washington DC Lehmann A A 2001 Direct and diffuse components of erythemal irradiance Measurements and modeling for clear sky conditions Ph D dissertation ETH No 14303 Swiss Federal Institute of Technology Zurich McKinley A F and Diffey B L 1987 A reference action spectrum for ultraviolet induced erythema in human skin CIE J 6 17 22 Myers D and Gueymard C 2004 Description and availability of the SMARTS spectral model for pho

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