2020A&A...642A..39R


Query : 2020A&A...642A..39R

2020A&A...642A..39R - Astronomy and Astrophysics, volume 642A, 39-39 (2020/10-1)

Dayside thermal inversion in the atmosphere of WASP-19b.

RAJPUROHIT A.S., ALLARD F., HOMEIER D., MOUSIS O. and RAJPUROHIT S.

Abstract (from CDS):


Context. Observations of ultra-hot Jupiters indicate the existence of thermal inversion in their atmospheres, with dayside temperatures greater than 2200 K. Various physical mechanisms such as non-local thermal equilibrium, cloud formation, disequilibrium chemistry, ionisation, hydrodynamic waves, and associated energy have been omitted in previous spectral retrievals, while they play an important role in the thermal structure of their upper atmospheres.
Aims. We aim to explore the atmospheric properties of WASP-19b to understand its largely featureless thermal spectra using a state-of-the-art atmosphere code that includes a detailed treatment of the most important physical and chemical processes at play in such atmospheres.
Methods. We used the one-dimensional line-by-line radiative transfer code PHOENIX in its spherical symmetry configuration including the BT-Settl cloud model and C/O disequilibrium chemistry to analyse the observed thermal spectrum of WASP-19b.
Results. We find evidence for a thermal inversion in the dayside atmosphere of the highly irradiated ultra-hot Jupiter WASP-19b, with Teq∼2700K. At these high temperatures we find that H2O dissociates thermally at pressures below 10–2 bar. The inverted temperature-pressure profiles of WASP-19b show evidence of CO emission features at 4.5µm in its secondary eclipse spectra.
Conclusions. We find that the atmosphere of WASP-19b is thermally inverted. We infer that the thermal inversion is due to the strong impinging radiation. We show that H2O is partially dissociated in the upper atmosphere above about τ=10–2, but is still a significant contributor to the infrared opacity, dominated by CO. The high-temperature and low-density conditions cause H2O to have a flatter opacity profile than in non-irradiated brown dwarfs. Altogether these factors make H2O more difficult to identify in WASP-19b. We suggest that the state-of-the-art PHOENIX model atmosphere code is well suited to the study of this new class of extrasolar planets, ultra-hot Jupiters.

Abstract Copyright: © ESO 2020

Journal keyword(s): radiative transfer - planets and satellites: gaseous planets - planets and satellites: atmospheres

Simbad objects: 12

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Number of rows : 12
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 KELT-1b Pl 00 01 26.9169325133 +39 23 01.782142922           ~ 93 0
2 HD 10069b Pl 01 37 25.0335097438 -45 40 40.376513381           ~ 310 1
3 HD 15082b Pl 02 26 51.0582746497 +37 33 01.737746137           ~ 286 1
4 WASP-12b Pl 06 30 32.7966788910 +29 40 20.266334158           G0 682 1
5 CD-38 3220b Pl 07 10 24.0606039387 -39 05 50.570553937           ~ 226 0
6 WASP-19b Pl 09 53 40.0764883458 -45 39 33.055979403           ~ 329 1
7 WASP-103b Pl 16 37 15.5753608801 +07 11 00.119024745           ~ 150 1
8 NAME BD+46 2629Ab Pl 19 07 53.1396671301 +46 52 05.931203366           ~ 142 1
9 BD+47 2846b Pl 19 28 59.3538131541 +47 58 10.216250846           ~ 337 1
10 HD 189733b Pl 20 00 43.7130382888 +22 42 39.071811263           ~ 1291 1
11 HD 195689b Pl 20 31 26.3534038246 +39 56 19.765154336           ~ 199 0
12 HD 209458b Pl 22 03 10.7729598762 +18 53 03.548248479           ~ 1707 1

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2022.10.01-12:57:48

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