Into the storm: diving into the winds of the ultra-hot Jupiter WASP-76 b with HARPS and ESPRESSO

被引：48

作者：

Seidel, J., V ^{[1
]}

Ehrenreich, D. ^{[1
]}

Allart, R. ^{[1
,2
,3
]}

Hoeijmakers, H. J. ^{[4
]}

Lovis, C. ^{[1
]}

Bourrier, V ^{[1
]}

Pino, L. ^{[5
]}

Wyttenbach, A. ^{[6
]}

Adibekyan, V ^{[7
,8
]}

Alibert, Y. ^{[9
,10
]}

Borsa, F. ^{[11
]}

Casasayas-Barris, N. ^{[15
,21
,22
]}

Cristiani, S. ^{[13
]}

Demangeon, O. D. S. ^{[7
,8
]}

Di Marcantonio, P. ^{[12
]}

Figueira, P. ^{[7
,14
]}

Gonzalez Hernandez, J., I ^{[15
]}

Lillo-Box, J. ^{[12
]}

Martins, C. J. A. P. ^{[7
,16
]}

Mehner, A. ^{[14
]}

Molaro, P. ^{[13
,20
]}

Nunes, N. J. ^{[17
]}

Palle, E. ^{[15
,21
]}

Pepe, F. ^{[1
]}

Santos, N. C. ^{[7
,8
]}

Sousa, S. G. ^{[7
]}

Sozzetti, A. ^{[18
]}

Tabernero, H. M. ^{[7
,19
]}

Zapatero Osorio, M. R. ^{[19
]}

机构：

[1] Univ Geneva, Observ Astron, Chemin Pegasi 51b, CH-1290 Versoix, Switzerland

[2] Univ Montreal, Dept Phys, Montreal, PQ H3T 1J4, Canada

[3] Univ Montreal, Inst Res Exoplanets, Montreal, PQ H3T 1J4, Canada

[4] Lund Observ, Box 43,Solvegatan 27, S-22100 Lund, Sweden

[5] INAF Osservatorio Astrofis Arcetri, Largo E Fermi 5, I-50125 Florence, Italy

[6] Univ Grenoble Alpes, IPAG, CNRS, F-38000 Grenoble, France

[7] Univ Porto, Inst Astrofis & Ciencias Espaco, CAUP, Rua Estrelas, P-4150762 Porto, Portugal

[8] Univ Porto, Fac Ciencias, Dept Fis & Astron, Rua Campo Alegre, P-4169007 Porto, Portugal

[9] Univ Bern, Phys Inst, CH-3012 Bern, Switzerland

[10] Univ Bern, NCCR PlanetS, CH-3012 Bern, Switzerland

[11] INAF Osservatorio Astron Brera, Via E Bianchi 46, I-23807 Merate, LC, Italy

[12] CSIC INTA, Dept Astrofis, Ctr Astrobiol CAB, ESAC Campus, Madrid 28692, Spain

[13] INAF Osservatorio Astron Trieste, Via Tiepolo 11, I-34143 Trieste, Italy

[14] European Southern Observ ESO, Alonso de Cordova 3107, Santiago, Chile

[15] Inst Astrofis Canarias, Via Lactea Sn, Tenerife 38200, Spain

[16] Univ Porto, Ctr Astrofis, Rua Estrelas, P-4150762 Porto, Portugal

[17] Univ Lisbon, Fac Ciencias, Inst Astrofis & Ciencias Espaco, P-1749016 Lisbon, Portugal

[18] INAF Osservatorio Astrofis Torino, Str Osservatorio 20, I-10025 Pino Torineseto, TO, Italy

[19] Ctr Astrobiol CSIC INTA, Ctra Ajalvir Km 4, Madrid 28850, Spain

[20] Inst Fundamental Phys IFPU, Via Beirut 2, I-34151 Grignano, TS, Italy

[21] Univ La Laguna, Dept Astrofis, San Cristobal De La Lagu 38200, Spain

[22] Leiden Univ, Leiden Observ, Postbus 9513, NL-2300 RA Leiden, Netherlands

来源：

ASTRONOMY & ASTROPHYSICS | 2021年 / 653卷 / 653期

基金：

欧洲研究理事会; 欧盟地平线“2020”; 瑞士国家科学基金会;

关键词：

planets and satellites: atmospheres; planets and satellites: individual: WASP-76 b; techniques: spectroscopic; line: profiles; methods: data analysis; RESOLUTION TRANSMISSION SPECTRUM; HD; 209458B; FE I; EXOPLANET; ATMOSPHERES; EMISSION; DAYSIDE; MODEL; PLANET; STARS;

D O I：

10.1051/0004-6361/202140569

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. Despite swift progress in the characterisation of exoplanet atmospheres in composition and structure, the study of atmospheric dynamics has not progressed at the same speed. While theoretical models have been developed to describe the lower layers of the atmosphere, and independently, the exosphere, little is known about the intermediate layers up to the thermosphere. Aims. We aim to provide a clearer picture of atmospheric dynamics for the class of ultra-hot Jupiters, which are highly irradiated gas giants, based on the example of WASP-76 b. Methods. We jointly analysed two datasets that were obtained with the HARPS and ESPRESSO spectrographs to interpret the resolved planetary sodium doublet. We then applied the MERC code, which retrieves wind patterns, speeds, and temperature profiles on the line shape of the sodium doublet. An updated version of MERC, with added planetary rotation, also provides the possibility of modelling the latitude dependence of the wind patterns. Results. We retrieve the highest Bayesian evidence for an isothermal atmosphere, interpreted as a mean temperature of 3389 +/- 227 K, a uniform day- to nightside wind of 5.5(-2.0)(+1.4) km s(-1) in the lower atmosphere with a vertical wind in the upper atmosphere of 22.7(-4.1)(+4.9) km s(-1), switching atmospheric wind patterns at 10(-3) bar above the reference surface pressure (10 bar). Conclusions. Our results for WASP-76 b are compatible with previous studies of the lower atmospheric dynamics of WASP-76 b and other ultra-hot Jupiters. They highlight the need for vertical winds in the intermediate atmosphere above the layers probed by global circulation model studies to explain the line broadening of the sodium doublet in this planet. This work demonstrates the capability of exploiting the resolved spectral line shapes to observationally constrain possible wind patterns in exoplanet atmospheres. This is an invaluable input to more sophisticated 3D atmospheric models in the future.

引用

页数：16

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