Atmospheric radiative transfer codes

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An atmospheric radiative transfer model, code, or simulator calculates

planetary atmosphere
.

Methods

At the core of a radiative transfer model lies the

monochromatic equation to calculate radiance in a single layer of the Earth's atmosphere. To calculate the radiance for a spectral region with a finite width (e.g., to estimate the Earth's energy budget or simulate an instrument response), one has to integrate this over a band of frequencies (or wavelengths). The most exact way to do this is to loop through the frequencies of interest, and for each frequency, calculate the radiance at this frequency. For this, one needs to calculate the contribution of each spectral line for all molecules in the atmospheric layer; this is called a line-by-line calculation. For an instrument response, this is then convolved
with the spectral response of the instrument.

A faster but more approximate method is a band transmission. Here, the transmission in a region in a band is characterised by a set of pre-calculated coefficients (depending on temperature and other parameters). In addition, models may consider scattering from molecules or particles, as well as polarisation; however, not all models do so.

Applications

Radiative transfer codes are used in broad range of applications. They are commonly used as forward models for the

radiation parameterization
. In these applications, the radiative transfer codes are used in forward sense, i.e. on the basis of known properties of the atmosphere, one calculates heating rates, radiative fluxes, and radiances.

There are efforts for intercomparison of radiation codes. One such project was ICRCCM (Intercomparison of Radiation Codes in Climate Models) effort that spanned the late 1980s – early 2000s. The more current (2011) project, Continual Intercomparison of Radiation Codes, emphasises also using observations to define intercomparison cases. [2]

Table of models

Name
 Website
 References
 UV
 Visible
 Near IR
 Thermal IR
 mm/sub-mm
 Microwave
 line-by-line/band
 Scattering
 Polarised
 Geometry
 License
 Notes
4A/OP [2] Archived 2011-07-21 at the Wayback Machine Scott and Chédin (1981)

[3]

No No Yes Yes No No band or line-by-line Yes Yes freeware
6S/6SV1 [3] Kotchenova et al. (1997)

[4]

No Yes Yes No No No band ? Yes non-Lambertian surface
ARTS [4] Eriksson et al. (2011)

[5]

Buehler et al. (2018) [6]

No No No Yes Yes Yes line-by-line Yes Yes spherical 1D, 2D, 3D
GPL
BTRAM [5] Chapman et al. (2009)

[7]

No Yes Yes Yes Yes Yes line-by-line No No 1D,plane-parallel proprietary commercial
COART [6] Jin et al. (2006)

[8]

Yes Yes Yes Yes No No Yes No plane-parallel free
CRM [7] No Yes Yes Yes No No band Yes No freely available Part of
NCAR
Community Climate Model
CRTM [8] Johnson et al. (2023)

[9]

v3.0 Yes Yes Yes Yes passive, active band Yes v3.0, UV/VIS 1D, Plane-Parallel Public Domain Fresnel ocean surfaces, Lambertian non-ocean surface
DART radiative transfer model [9] Gastellu-Etchegorry et al. (1996)

[10]

No Yes Yes Yes No No band Yes ? spherical 1D, 2D, 3D free for research with license non-Lambertian surface, landscape creation and import
DISORT [10] Stamnes et al. (1988)[11]

Lin et al. (2015)[12]

Yes Yes Yes Yes Yes radar Yes No plane-parallel or pseudo-spherical (v4.0) free with restrictions discrete ordinate, used by others
Eradiate [11] No Yes Yes No No No band or line-by-line Yes No plane-parallel, spherical LGPL 3D surface simulation
FARMS [12] Xie et al. (2016)

[13]

λ>0.2 µm Yes Yes No No No band Yes No plane-parallel free Rapidly simulating downwelling solar radiation at land surface for solar energy and climate research
Fu-Liou [13] Fu and Liou (1993)

[14]

No Yes Yes ? No No Yes ? plane-parallel usage online, source code available web interface online at [15]
FUTBOLIN Martin-Torres (2005)

[16]

λ>0.3 µm Yes Yes Yes λ<1000 µm No line-by-line Yes ? spherical or plane-parallel handles line-mixing, continuum absorption and NLTE
GENLN2 [14] Edwards (1992)

[17]

? ? ? Yes ? ? line-by-line ? ?
KARINE [15] Eymet (2005)

[18]

No No Yes No No ? ? plane-parallel GPL
KCARTA [16] ? ? Yes Yes ? ? line-by-line Yes ? plane-parallel freely available
AIRS
reference model
KOPRA [17] No No No Yes No No ? ?
LBLRTM [18] Clough et al. (2005)

[19]

Yes Yes Yes Yes Yes Yes line-by-line ? ?
LEEDR [19] Fiorino et al. (2014)

[20]

λ>0.2 µm Yes Yes Yes Yes Yes band or line-by-line Yes ? spherical US government software extended solar & lunar sources;

single & multiple scattering

LinePak [20] Gordley et al. (1994)

[21]

Yes Yes Yes Yes Yes Yes line-by-line No No spherical (Earth and Mars), plane-parallel freely available with restrictions web interface, SpectralCalc
libRadtran [21] Mayer and Kylling (2005)

[22]

Yes Yes Yes Yes No No band or line-by-line Yes Yes plane-parallel or pseudo-spherical
GPL
MATISSE [22] Caillault et al. (2007)

[23]

No Yes Yes Yes No No band Yes ? proprietary freeware
MCARaTS [24] GPL 3-D Monte Carlo
MODTRAN [23] Berk et al. (1998)

[25]

ṽ
<50,000 cm−1 (eq. to λ>0.2 µm) 		Yes Yes Yes Yes Yes band or line-by-line Yes ? proprietary commercial solar and lunar source, uses DISORT
MOSART [24] Cornette (2006)

[26]

λ>0.2 µm Yes Yes Yes Yes Yes band Yes No freely available
MSCART [25] Wang et al. (2017)[27]

Wang et al. (2019)[28]

Yes Yes Yes No No No Yes Yes 1D, 2D, 3D available on request
PICASO [26]link Batalha et al. (2019)[29] Mukherjee et al. (2022)[30] λ>0.3 μm Yes Yes Yes No No band or correlated-k Yes No plane-parallel, 1D, 3D GPL Github exoplanet, brown dwarf, climate modeling, phase-dependence
PUMAS [27] Yes Yes Yes Yes Yes Yes Line-by-line and correlated-k Yes Yes plane-parallel and pseudo-spherical Free/online tool
RADIS [28] Pannier (2018)

[31]

No No Yes No No No No 1D GPL
RFM [29] No No No Yes No No line-by-line No ? available on request
MIPAS
reference model based on GENLN2
RRTM/RRTMG
 [30] Mlawer, et al. (1997)

[32]

ṽ
<50,000 cm−1 (eq. to λ>0.2 µm) 		Yes Yes Yes Yes
ṽ
>10 cm−1 		? ? free of charge uses DISORT
RTMOM [31][dead link] λ>0.25 µm Yes Yes λ<15 µm No No line-by-line Yes ? plane-parallel freeware
RTTOV [32] Saunders et al. (1999)

[33]

λ>0.4 µm Yes Yes Yes Yes Yes band Yes ? available on request
SASKTRAN [34] Bourassa et al.

(2008)[35]

Zawada et al.

(2015)[36]

Yes Yes Yes No No No line-by-line Yes Yes spherical 1D, 2D, 3D, plane-parallel available on request discrete and Monte Carlo options
SBDART [33] Ricchiazzi et al. (1998)

[37]

Yes Yes Yes ? No No Yes ? plane-parallel uses DISORT
SCIATRAN [34] Rozanov et al. (2005)

,[38] 

Rozanov et al. (2014)

[39]

Yes Yes Yes No No No band or line-by-line Yes Yes plane-parallel or pseudo-spherical or spherical
SHARM Lyapustin (2002)

[40]

No Yes Yes No No No Yes ?
SHDOM [35] Evans (2006)

[41]

? ? Yes Yes ? ? Yes ?
σ-IASI [36] Amato et al. (2002)[42]

Liuzzi et al. (2017)[43]

No No Yes Yes Yes No band Yes No plane-parallel Available on request Semi-analytical Jacobians.
SMART-G [37] Ramon et al. (2019)

[44]

Yes Yes Yes No No No band or line-by-line Yes Yes plane-parallel or spherical free for non-commercial purposes Monte-Carlo code parallelized by GPU (CUDA). Atmosphere or/and ocean options
Streamer, Fluxnet [38][45] Key and Schweiger (1998)

[46]

No No λ>0.6 mm λ<15 mm No No band Yes ? plane-parallel Fluxnet is fast version of STREAMER using
neural nets
XRTM [39] Yes Yes Yes Yes Yes Yes Yes Yes plane-parallel and pseudo-spherical GPL
VLIDORT/LIDORT [40][47] Spurr and Christi (2019)

[48]

Yes Yes Yes Yes ? ? line-by-line Yes Yes VLIDORT only plane-parallel Used in SMART and VSTAR radiative transfer
Name Website References UV VIS Near IR Thermal IR Microwave mm/sub-mm line-by-line/band Scattering Polarised Geometry License Notes

Molecular absorption databases

For a line-by-line calculation, one needs characteristics of the spectral lines, such as the line centre, the intensity, the lower-state energy, the line width and the shape.

Name Author Description
HITRAN[49] Rothman et al. (1987, 1992, 1998, 2003, 2005, 2009, 2013, 2017) HITRAN is a compilation of molecular spectroscopic parameters that a variety of computer codes use to predict and simulate the transmission and emission of light in the atmosphere. The original version was created at the Air Force Cambridge Research Laboratories (1960's). The database is maintained and developed at the Harvard-Smithsonian Center for Astrophysics in Cambridge MA, USA.
GEISA[50] Jacquinet-Husson et al. (1999, 2005, 2008) GEISA (Gestion et Etude des Informations Spectroscopiques Atmosphériques: Management and Study of Spectroscopic Information) is a computer-accessible spectroscopic database, designed to facilitate accurate forward radiative transfer calculations using a line-by-line and layer-by-layer approach. It was started in 1974 at Laboratoire de Météorologie Dynamique (LMD/IPSL) in France. GEISA is maintained by the ARA group at LMD (Ecole Polytechnique) for its scientific part and by the ETHER group (CNRS Centre National de la Recherche Scientifique-France) at IPSL (Institut Pierre Simon Laplace) for its technical part. Currently, GEISA is involved in activities related to the assessment of the capabilities of IASI (
Infrared Atmospheric Sounding Interferometer
on board of the METOP European satellite) through the GEISA/IASI database derived from GEISA.

See also

References

Footnotes
  1. doi:10.1016/j.solener.2013.01.030
    .
  2. ^ Continual Intercomparison of Radiation Codes
  3. doi:10.1175/1520-0450(1981)020<0802:AFLBLM>2.0.CO;2
    .
  4. PMID 16926910
    .
  5. doi:10.1016/j.jqsrt.2011.03.001
    . Retrieved 2016-11-02.
  6. doi:10.5194/gmd-11-1537-2018
    . Retrieved 2023-01-16.
  7. ^ Chapman, I. M.; Naylor, D. A.; Gom, B. G.; Querel, R. R.; Davis-Imhof, P. (2009). "BTRAM: An Interactive Atmospheric Radiative Transfer Model". The 30th Canadian Symposium on Remote Sensing. 30: 22–25.
  8. S2CID 39305812
    .
  9. S2CID 258738740
    .
  10. doi:10.1016/0034-4257(95)00253-7
    .
  11. PMID 20531783
    .
  12. S2CID 119467744
    .
  13. doi:10.1016/j.solener.2016.06.003
    .
  14. doi:10.1175/1520-0469(1993)050<2008:POTRPO>2.0.CO;2
    .
  15. ^ "Fu-Liou Cloud/Aerosol Forcing Page (Version 200503/MARCH 2005)". Langley Research Center. NASA. Archived from the original on 2010-05-27. Retrieved 2010-07-07.
  16. Bibcode:2003EAEJA.....7735M
    .
  17. ^ Edwards, D. P. (1992), GENLN2: A general line-by-line atmospheric transmittance and radiance model, Version 3.0 description and users guide, NCAR/TN-367-STR, National Center for Atmospheric Research, Boulder, Co.
  18. ^ KARINE: a tool for infrared radiative transfer analysis in planetary atmospheres par V. Eymet. Note technique interne, Laboratoire d'Energétique, 2005.
  19. hdl:2027.42/142162
    .
  20. doi:10.1175/JAMC-D-13-036.1
    .
  21. doi:10.1016/0022-4073(94)90025-6
    .
  22. doi:10.5194/acp-5-1855-2005
    .
  23. PMID 17676164
    .
  24. ^ "MCARaTS". sites.google.com. Retrieved 2016-04-01.
  25. doi:10.1016/S0034-4257(98)00045-5
    .
  26. ^ Cornette, William M. (2006). "Moderate Spectral Atmospheric Radiance and Transmittance (MOSART) Computer Code Version 2.00., Lexington, MA (2006)". Proc. IEEE-GRSS/AFRL Atmospheric Transmission Modeling Conference, Lexington MA.
  27. doi:10.1016/j.jqsrt.2016.12.002
    .
  28. doi:10.1016/j.jqsrt.2019.06.025
    .
  29. S2CID 128347336
    .
  30. S2CID 251594505
    .
  31. S2CID 125474810
    .
  32. S2CID 54031652
    .
  33. doi:10.1256/smsqj.55614
    .
  34. ^ "Welcome to SASKTRAN's documentation! — SASKTRAN 0.1.3 documentation". arg.usask.ca. Retrieved 2018-04-11.
  35. doi:10.1016/j.jqsrt.2007.07.007
    .
  36. ISSN 1867-8548
    .
  37. S2CID 55800532
    .
  38. doi:10.1016/j.asr.2005.03.012
    .
  39. doi:10.1016/j.jqsrt.2013.07.004
    .
  40. PMID 12269559
    .
  41. S2CID 40027059
    .
  42. doi:10.1016/S1364-8152(02)00027-0
    .
  43. hdl:11563/125342
    .
  44. S2CID 125121586
    .
  45. ^ FluxNet
  46. S2CID 118079586
    .
  47. ^ [1] |-->]
  48. S2CID 126425750
    .
  49. ^ HITRAN Site
  50. ^ GEISA Site
General

External links
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