Query : 2013A&A...551A.131V

2013A&A...551A.131V - Astronomy and Astrophysics, volume 551A, 131-131 (2013/3-1)

High-temperature measurements of VUV-absorption cross sections of CO2 and their application to exoplanets.


Abstract (from CDS):

Ultraviolet (UV) absorption cross sections are an essential ingredient of photochemical atmosphere models. Exoplanet searches have unveiled a large population of short-period objects with hot atmospheres, very different from what we find in our solar system. Transiting exoplanets whose atmospheres can now be studied by transit spectroscopy receive extremely strong UV fluxes and have typical temperatures ranging from 400 to 2500K. At these temperatures, UV photolysis cross section data are severely lacking. Our goal is to provide high-temperature absorption cross sections and their temperature dependency for important atmospheric compounds. This study is dedicated to CO2, which is observed and photodissociated in exoplanet atmospheres. We also investigate the influence of these new data on the photochemistry of some exoplanets. We performed these measurements with synchrotron radiation as a tunable VUV light source for the 115-200nm range at 300, 410, 480, and 550K. In the 195-230nm range, we used a deuterium lamp and a 1.5m Jobin-Yvon spectrometer and we worked at seven temperatures between 465 and 800K. We implemented the measured cross section into a 1D photochemical model. For λ>170nm, the wavelength dependence of ln(σCO2(λ,T)x1/Qv(T) can be parametrized with a linear law. Thus, we can interpolate σCO2(λ,T) at any temperature between 300 and 800K. Within the studied range of temperature, the CO2 cross section can vary by more than two orders of magnitude. This, in particular, makes the absorption of CO2 significant up to wavelengths as high as 230nm, while it is negligible above 200nm at 300 K. The absorption cross section of CO2 is very sensitive to temperature, especially above 160nm. The model predicts that accounting for this temperature dependency of CO2 cross section can affect the computed abundances of NH3, CO2, and CO by one order of magnitude in the atmospheres of hot Jupiter and hot Neptune. This effect will be more important in hot CO2-dominated atmospheres.

Abstract Copyright:

Journal keyword(s): molecular data - planets and satellites: atmospheres - methods: laboratory

Simbad objects: 6

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Number of rows : 6
N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
1 HD 31253b Pl 04 54 43.6536626593 +12 21 07.899766290           ~ 10 1
2 Ross 905b Pl 11 42 11.0933874353 +26 42 23.658083337           ~ 732 1
3 * sig Boo PM* 14 34 40.8173867232 +29 44 42.457673940 4.76 4.84 4.47 4.13 3.94 F4VkF2mF1 589 0
4 HD 152751 SB* 16 55 28.7575690 -08 20 10.787849 11.647 10.593 9.023 7.937 6.565 M3.5Ve 509 1
5 HD 153950b Pl 17 04 30.8709230438 -43 18 35.170476437           ~ 11 1
6 HD 221287b Pl 23 31 20.3381873379 -58 12 35.032427169           ~ 21 1

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