Difference between revisions of "Rayleigh scattering"
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== About Rayleigh scattering == | == About Rayleigh scattering == | ||
| − | http://web.gps.caltech.edu/~vijay/Papers/Rayleigh_Scattering/Bodhaine-etal-99.pdf | + | The following article gives a clear overview on Rayleigh scattering cross sections : |
| + | |||
| + | ''Bodhaine'' (1999) On Rayleigh Optical Depth Calculations : http://web.gps.caltech.edu/~vijay/Papers/Rayleigh_Scattering/Bodhaine-etal-99.pdf | ||
| + | |||
| + | Have a look especially on equations (2) and (9). | ||
== About Rayleigh scattering in LMDZ Generic == | == About Rayleigh scattering in LMDZ Generic == | ||
| Line 9: | Line 13: | ||
=== LMDZ === | === LMDZ === | ||
| − | ''Hansen'' (1974) : https://ui.adsabs.harvard.edu/link_gateway/1974SSRv...16..527H/ADS_PDF equations (2.29) to (2.32) | + | LMDZ uses formalism from : |
| + | |||
| + | ''Hansen'' (1974) Light scattering in planetary atmospheres : https://ui.adsabs.harvard.edu/link_gateway/1974SSRv...16..527H/ADS_PDF | ||
| + | |||
| + | Have a look on equations (2.29) to (2.32). | ||
=== exo_k === | === exo_k === | ||
| − | Rayleigh routine in exo_k : http://perso.astrophy.u-bordeaux.fr/~jleconte/exo_k-doc/_modules/exo_k/rayleigh.html#Rayleigh.sigma_mol | + | Rayleigh routine in exo_k is avalaible here : |
| + | |||
| + | http://perso.astrophy.u-bordeaux.fr/~jleconte/exo_k-doc/_modules/exo_k/rayleigh.html#Rayleigh.sigma_mol | ||
Exo_k uses formalism from : | Exo_k uses formalism from : | ||
| − | ''Caldas'' (2019) : https://hal.archives-ouvertes.fr/hal-02005332/document equation (12) & appendix D | + | |
| + | ''Caldas'' (2019) Effects of a fully 3D atmospheric structure on exoplanet transmission spectra: retrieval biases due to day–night temperature gradients : https://hal.archives-ouvertes.fr/hal-02005332/document | ||
| + | |||
| + | Have a look on equation (12) & appendix D | ||
== Formalism == | == Formalism == | ||
| − | We consider a layer . | + | We consider a layer. |
| − | + | dP is the difference of pressure between the two levels that define the layer. | |
| − | dm is the mass per m2 of the layer | + | dN is the number of molecules per m2 & dm is the mass per m2 of the layer |
| − | + | dTau is the optical depth for a given wavelength (or wavenumber) | |
| + | |||
| + | <math>m_{molecule}</math> is the mass of one molecule of the considered gas | ||
| + | |||
| + | g is the gravity | ||
| + | |||
| + | sigma_mol is the Rayleigh scattering cross section of the molecule | ||
=== LMDZ formalism === | === LMDZ formalism === | ||
| − | + | dTau = (tauconsti * tauvari) * dP | |
| + | |||
| + | tauvari = tauvari(wavelength in microns) | ||
| − | + | dP here is in mBar | |
=== exo_k formalism === | === exo_k formalism === | ||
| − | + | dTau = sigma_mol * dN | |
| − | + | sigma_mol = sigma_mol(wavenumber in cm-1) | |
| − | and then : | + | which gives : dTau = sigma_mol <math> \displaystyle \frac{dm}{m_{molecule}} </math> |
| + | |||
| + | and then : dTau <math> \displaystyle = \frac{\text{sigma_mol}}{g * m_{molecule}} dP</math> | ||
| + | |||
| + | dP here is in Pascal | ||
=== Relations between LMDZ & Exo_k formalisms === | === Relations between LMDZ & Exo_k formalisms === | ||
| Line 46: | Line 71: | ||
LMDZ & exo_k formalism are linked as following : | LMDZ & exo_k formalism are linked as following : | ||
| − | <math> \displaystyle \text{ | + | <math> \displaystyle \text{(tauconsti * tauvari)} = \frac{\text{sigma_mol}}{g * m_{molecule}} * \text{scalep}</math> |
| − | Be careful with units !!! (cm-1 for wavenumbers in exo_k, microns for wavelengths in LMDZ | + | Be careful with units !!! (cm-1 for wavenumbers in exo_k, microns for wavelengths in LMDZ) |
| + | |||
| + | Last but not least : not to forget the ''scalep'' factor in LMDZ ! | ||
| + | scalep = 100, because P is in mBar in optcv.F90 . | ||
| + | So we move from Pascal to mBar | ||
=== To be noticed === | === To be noticed === | ||
| − | TAURAY(NW) is calculated in calc_rayleigh.F90. | + | TAURAY(NW) is calculated in calc_rayleigh.F90 for a given channel NW. |
| − | + | TAUVAR is first calculated, and then averaged by the black body function for each channel to give TAURAY : | |
<math> \text{TAURAY(NW)} = \frac{\int_{\lambda' \in \text{channel}} \text{TAUVAR} (\lambda') B_{\lambda} \, \mathrm{d}\lambda'}{\int B_{\lambda} \, \mathrm{d}\lambda'} </math> | <math> \text{TAURAY(NW)} = \frac{\int_{\lambda' \in \text{channel}} \text{TAUVAR} (\lambda') B_{\lambda} \, \mathrm{d}\lambda'}{\int B_{\lambda} \, \mathrm{d}\lambda'} </math> | ||
| − | TAUVAR is cut into two parts : TAUCONSTI et TAUVARI with TAUVAR = TAUCONSTI * TAUVARI | + | TAUVAR is cut into two parts : TAUCONSTI et TAUVARI (previously mentionned) with TAUVAR = TAUCONSTI * TAUVARI |
The <math> \lambda </math> dependence is in the TAUVARI | The <math> \lambda </math> dependence is in the TAUVARI | ||
| + | |||
| + | [[Category:Generic-Model]] | ||
Latest revision as of 11:17, 9 March 2023
Contents
About Rayleigh scattering
The following article gives a clear overview on Rayleigh scattering cross sections :
Bodhaine (1999) On Rayleigh Optical Depth Calculations : http://web.gps.caltech.edu/~vijay/Papers/Rayleigh_Scattering/Bodhaine-etal-99.pdf
Have a look especially on equations (2) and (9).
About Rayleigh scattering in LMDZ Generic
References
LMDZ
LMDZ uses formalism from :
Hansen (1974) Light scattering in planetary atmospheres : https://ui.adsabs.harvard.edu/link_gateway/1974SSRv...16..527H/ADS_PDF
Have a look on equations (2.29) to (2.32).
exo_k
Rayleigh routine in exo_k is avalaible here :
Exo_k uses formalism from :
Caldas (2019) Effects of a fully 3D atmospheric structure on exoplanet transmission spectra: retrieval biases due to day–night temperature gradients : https://hal.archives-ouvertes.fr/hal-02005332/document
Have a look on equation (12) & appendix D
Formalism
We consider a layer.
dP is the difference of pressure between the two levels that define the layer.
dN is the number of molecules per m2 & dm is the mass per m2 of the layer
dTau is the optical depth for a given wavelength (or wavenumber)
\(m_{molecule}\) is the mass of one molecule of the considered gas
g is the gravity
sigma_mol is the Rayleigh scattering cross section of the molecule
LMDZ formalism
dTau = (tauconsti * tauvari) * dP
tauvari = tauvari(wavelength in microns)
dP here is in mBar
exo_k formalism
dTau = sigma_mol * dN
sigma_mol = sigma_mol(wavenumber in cm-1)
which gives : dTau = sigma_mol \( \displaystyle \frac{dm}{m_{molecule}} \)
and then : dTau \( \displaystyle = \frac{\text{sigma_mol}}{g * m_{molecule}} dP\)
dP here is in Pascal
Relations between LMDZ & Exo_k formalisms
LMDZ & exo_k formalism are linked as following \[ \displaystyle \text{(tauconsti * tauvari)} = \frac{\text{sigma_mol}}{g * m_{molecule}} * \text{scalep}\]
Be careful with units !!! (cm-1 for wavenumbers in exo_k, microns for wavelengths in LMDZ)
Last but not least : not to forget the scalep factor in LMDZ ! scalep = 100, because P is in mBar in optcv.F90 . So we move from Pascal to mBar
To be noticed
TAURAY(NW) is calculated in calc_rayleigh.F90 for a given channel NW.
TAUVAR is first calculated, and then averaged by the black body function for each channel to give TAURAY \[ \text{TAURAY(NW)} = \frac{\int_{\lambda' \in \text{channel}} \text{TAUVAR} (\lambda') B_{\lambda} \, \mathrm{d}\lambda'}{\int B_{\lambda} \, \mathrm{d}\lambda'} \]
TAUVAR is cut into two parts : TAUCONSTI et TAUVARI (previously mentionned) with TAUVAR = TAUCONSTI * TAUVARI
The \( \lambda \) dependence is in the TAUVARI
