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J/ApJ/832/30     Raman scattering cross sections for H2     (Oklopcic+, 2016)

Raman scattering by molecular hydrogen and nitrogen in exoplanetary atmospheres. Oklopcic A., Hirata C.M., Heng K. <Astrophys. J., 832, 30-30 (2016)> =2016ApJ...832...30O (SIMBAD/NED BibCode)
ADC_Keywords: Atomic physics Keywords: molecular processes; planets and satellites: atmospheres; radiative transfer; scattering; techniques: spectroscopic Abstract: An important source of opacity in exoplanet atmospheres at short visible and near-UV wavelengths is Rayleigh scattering of light on molecules. It is accompanied by a related, albeit weaker process-Raman scattering. We analyze the signatures of Raman scattering imprinted in the reflected light and the geometric albedo of exoplanets, which could provide information about atmospheric properties. Raman scattering affects the geometric albedo spectra of planets in the following ways. First, it causes filling-in of strong absorption lines in the incident radiation, thus producing sharp peaks in the albedo. Second, it shifts the wavelengths of spectral features in the reflected light causing the so-called Raman ghost lines. Raman scattering can also cause a broadband reduction of the albedo due to wavelength shifting of a stellar spectrum with red spectral index. Observing the Raman peaks in the albedo could be used to measure the column density of gas, thus providing constraints on the presence of clouds in the atmosphere. Observing the Raman ghost lines could be used to spectroscopically identify the main scatterer in the atmosphere, even molecules like H2 or N2, which do not have prominent spectral signatures in the optical wavelength range. If detected, ghost lines could also provide information about the temperature of the atmosphere. In this paper, we investigate the effects of Raman scattering in hydrogen- and nitrogen-dominated atmospheres. We analyze the feasibility of detecting the signatures of Raman scattering with the existing and future observational facilities, and of using these signatures as probes of exoplanetary atmospheres. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 38 56 Raman scattering cross sections for H2
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1 I1 --- Ji [0/9] Initial rotational quantum number for ground vibrational level 3- 4 I2 --- Jf [0/11] Final rotational quantum number 6 I1 --- vf [0/1] Final vibrational quantum number 8- 24 E17.10 cm+6 CS [4e-48/10e-45] Cross section coefficient 26- 38 F13.7 cm-1 delnu [-1815.5/5927.8] Raman shift
History: From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 15-Feb-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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