2018A&A...617A.110P


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.03CEST23:12:33

2018A&A...617A.110P - Astronomy and Astrophysics, volume 617A, 110-110 (2018/9-1)

From thermal dissociation to condensation in the atmospheres of ultra hot Jupiters: WASP-121b in context.

PARMENTIER V., LINE M.R., BEAN J.L., MANSFIELD M., KREIDBERG L., LUPU R., VISSCHER C., DESERT J.-M., FORTNEY J.J., DELEUIL M., ARCANGELI J., SHOWMAN A.P. and MARLEY M.S.

Abstract (from CDS):


Context. A new class of exoplanets has emerged: the ultra hot Jupiters, the hottest close-in gas giants. The majority of them have weaker-than-expected spectral features in the 1.1-1.7µm bandpass probed by HST/WFC3 but stronger spectral features at longer wavelengths probed by Spitzer. This led previous authors to puzzling conclusions about the thermal structures and chemical abundances of these planets.
Aims. We investigate how thermal dissociation, ionization, H opacity, and clouds shape the thermal structures and spectral properties of ultra hot Jupiters.
Methods. We use the SPARC/MITgcm to model the atmospheres of four ultra hot Jupiters and discuss more thoroughly the case of WASP-121b. We expand our findings to the whole population of ultra hot Jupiters through analytical quantification of the thermal dissociation and its influence on the strength of spectral features.
Results. We predict that most molecules are thermally dissociated and alkalies are ionized in the dayside photospheres of ultra hot Jupiters. This includes H2O, TiO, VO, and H2 but not CO, which has a stronger molecular bond. The vertical molecular gradient created by the dissociation significantly weakens the spectral features from H2O while the 4.5µm CO feature remains unchanged. The water band in the HST/WFC3 bandpass is further weakened by the continuous opacity of the H ions. Molecules are expected to recombine before reaching the limb, leading to order of magnitude variations of the chemical composition and cloud coverage between the limb and the dayside.
Conclusions. Molecular dissociation provides a qualitative understanding of the lack of strong spectral features of water in the 1-2µm bandpass observed in most ultra hot Jupiters. Quantitatively, our model does not provide a satisfactory match to the WASP-121b emission spectrum. Together with WASP-33b and Kepler-33Ab, they seem the outliers among the population of ultra hot Jupiters, in need of a more thorough understanding.

Abstract Copyright: © ESO 2018

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

Simbad objects: 19

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Number of rows : 19

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 KELT-1b Pl 00 01 26.9169325133 +39 23 01.782142922           ~ 61 0
2 HD 10069b Pl 01 37 25.0335097438 -45 40 40.376513381           ~ 211 1
3 HAT-P-32b Pl 02 04 10.2775457769 +46 41 16.210382751           ~ 82 1
4 HD 15082b Pl 02 26 51.0582746497 +37 33 01.737746137           ~ 181 1
5 WASP-12b Pl 06 30 32.7966788910 +29 40 20.266334158           G0 534 1
6 CD-38 3220b Pl 07 10 24.0606039387 -39 05 50.570553937           ~ 88 0
7 CD-38 3220 * 07 10 24.0606039387 -39 05 50.570553937   11.00 10.51     F6V 31 0
8 WASP-19b Pl 09 53 40.0764883458 -45 39 33.055979403           ~ 246 1
9 WASP-43b Pl 10 19 38.0089444408 -09 48 22.603103969           ~ 193 1
10 WASP-103b Pl 16 37 15.5753608801 +07 11 00.119024745           ~ 81 1
11 TrES-3 Pl 17 52 07.0185036683 +37 32 46.237002085           ~ 192 2
12 NAME BD+46 2629Ab Pl 19 07 53.1396671301 +46 52 05.931203366           ~ 107 1
13 CoRoT-2b Pl 19 27 06.4944821296 +01 23 01.357597206           ~ 178 1
14 BD+47 2846b Pl 19 28 59.3538131541 +47 58 10.216250846           ~ 268 1
15 HD 189733b Pl 20 00 43.7130382888 +22 42 39.071811263           ~ 1082 1
16 HD 195689b Pl 20 31 26.3534038246 +39 56 19.765154336           ~ 79 0
17 HD 201585b Pl 21 10 12.3723474386 +10 44 19.944718883           ~ 14 0
18 HD 209458b Pl 22 03 10.7729598762 +18 53 03.548248479           ~ 1468 1
19 WASP-4b Pl 23 34 15.0858223039 -42 03 41.049468209           ~ 117 1

    Equat.    Gal    SGal    Ecl

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2020.07.03-23:12:33

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