The GAPS Programme at TNG XXXI. The WASP-33 system revisited with HARPS-N

被引：24

作者：

Borsa, F. ^{[1
]}

Lanza, A. F. ^{[2
]}

Raspantini, I ^{[3
]}

Rainer, M. ^{[4
]}

Fossati, L. ^{[5
]}

Brogi, M. ^{[6
,7
,8
]}

Di Mauro, M. P. ^{[9
]}

Gratton, R. ^{[10
]}

Pino, L. ^{[4
]}

Benatti, S. ^{[11
]}

Bignamini, A. ^{[12
]}

Bonomo, A. S. ^{[7
]}

Claudi, R. ^{[10
]}

Esposito, M. ^{[13
]}

Frustagli, G. ^{[1
,3
]}

Maggio, A. ^{[11
]}

Maldonado, J. ^{[11
]}

Mancini, L. ^{[7
,14
,15
]}

Micela, G. ^{[11
]}

Nascimbeni, V ^{[10
]}

Poretti, E. ^{[1
,16
]}

Scandariato, G. ^{[2
]}

Sicilia, D. ^{[2
]}

Sozzetti, A. ^{[7
]}

Boschin, W. ^{[16
,17
,18
]}

Cosentino, R. ^{[16
]}

Covino, E. ^{[19
]}

Desidera, S. ^{[10
]}

Di Fabrizio, L. ^{[16
]}

Fiorenzano, A. F. M. ^{[16
]}

Harutyunyan, A. ^{[16
]}

Knapic, C. ^{[12
]}

Molinari, E. ^{[20
]}

Pagano, I ^{[2
]}

Pedani, M. ^{[16
]}

Piotto, G. ^{[21
]}

机构：

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

[2] INAF Osservatorio Astrofis Catania, Via S Sofia 78, I-95123 Catania, Italy

[3] Univ Milano Bicocca, Dipartimento Fis, Piazza Ateneo Nuovo 1, I-20126 Milan, Italy

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

[5] Austrian Acad Sci, Space Res Inst, Schmiedl Str 6, A-8042 Graz, Austria

[6] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England

[7] INAF Osservatorio Astrofis Torino, Via Osservatorio 20, I-10025 Pino Torinese, Italy

[8] Univ Warwick, Ctr Exoplanets & Habitabil, Gibbet Hill Rd, Coventry CV4 7AL, W Midlands, England

[9] INAF IAPS Ist Astrofis & Planetol Spaziali, Via Fosso Cavaliere 100, I-00133 Rome, Italy

[10] INAF Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy

[11] INAF Osservatorio Astron Palermo, Piazza Parlamento 1, I-90134 Palermo, Italy

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

[13] Thuringer Landessternwarte Tautenburg, Sternwarte 5, D-07778 Tautenburg, Germany

[14] Univ Roma Tor Vergata, Dept Phys, Via Ric Sci 1, I-00133 Rome, Italy

[15] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany

[16] Fdn Galileo Galilei INAF, Rambla Jose Ana Fernandez Perez 7, Brena Baja 38712, TF, Spain

[17] Inst Astrofis Canarias IAC, C Via Lactea S-N, San Cristobal la Laguna 38205, TF, Spain

[18] Univ La Laguna ULL, Dept Astrofis, San Cristobal la Laguna 38206, TF, Spain

[19] INAF Osservatorio Astron Capodimonte, Salita Moiariello 16, I-80131 Naples, Italy

[20] INAF Osservatorio Cagliari, Via Sci 5, I-09047 Selargius, CA, Italy

[21] Univ Padua, Dip Fis & Astron Galileo Galilei, Vicolo Osservatorio 2, I-35122 Padua, Italy

来源：

ASTRONOMY & ASTROPHYSICS | 2021年 / 653卷

关键词：

techniques: spectroscopic; planetary systems; planets and satellites: atmospheres; stars: individual: WASP-33; techniques: radial velocities; LINE-PROFILE TOMOGRAPHY; TO-LIMB VARIATION; TRANSMISSION SPECTRUM; DAYSIDE ATMOSPHERE; EXOPLANET TRANSITS; HOT; STELLAR; STARS; MASS; EVOLUTION;

D O I：

10.1051/0004-6361/202140559

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. Giant planets in short-period orbits around bright stars represent optimal candidates for atmospheric and dynamical studies of exoplanetary systems. Aims. We aim to analyse four transits of WASP-33b observed with the optical high-resolution HARPS-N spectrograph to confirm its nodal precession, study its atmosphere, and investigate the presence of star-planet interactions. Methods. We extracted the mean line profiles of the spectra using the least-squares deconvolution method, and we analysed the Doppler shadow and the radial velocities. We also derived the transmission spectrum of the planet, correcting it for the stellar contamination due to rotation, centre-to-limb variations, and pulsations. Results. We confirm the previously discovered nodal precession of WASP-33b, almost doubling the time coverage of the inclination and projected spin-orbit angle variation. We find that the projected obliquity reached a minimum in 2011, and we used this constraint to derive the geometry of the system, and in particular its obliquity at that epoch (epsilon = 113.99 degrees +/- 0.22 degrees) and the inclination of the stellar spin axis (i(s) = 90.11 degrees +/- 0.12 degrees). We also derived the gravitational quadrupole moment of the star J(2) = (6.73 +/- 0.22) x 10(-5), which we find to be in close agreement with the theoretically predicted value. Small systematics errors are computed by shifting the date of the minimum projected obliquity. We present detections of H alpha and H beta absorption in the atmosphere of the planet, with a contrast almost twice as small as that previously detected in the literature. We also find evidence for the presence of a pre-transit signal, which repeats in all four analysed transits and should thus be related to the planet. The most likely explanation lies in a possible excitation of a stellar pulsation mode by the presence of the planetary companion. Conclusions. A future common analysis of all available datasets in the literature will help shed light on the possibility that the observed Balmer lines' transit depth variations are related to stellar activity and pulsation, and to set constraints on the planetary temperature-pressure structure and thus on the energetics possibly driving atmospheric escape. A complete orbital phase coverage of WASP-33b with high-resolution spectroscopic (and spectro-polarimetric) observations could help us to understand the nature of the pre-transit signal.

引用

页数：17

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