The retrograde orbit of the HAT-P-6b exoplanet

被引：64

作者：

Hebrard, G. ^{[1
,2
]}

Ehrenreich, D. ^{[3
]}

Bouchy, F. ^{[1
,2
]}

Delfosse, X. ^{[3
]}

Moutou, C. ^{[4
]}

Arnold, L. ^{[2
]}

Boisse, I. ^{[1
,5
]}

Bonfils, X. ^{[3
]}

Diaz, R. F. ^{[1
,2
]}

Eggenberger, A. ^{[3
]}

Forveille, T. ^{[3
]}

Lagrange, A-M ^{[3
]}

Lovis, C. ^{[6
]}

Pepe, F. ^{[6
]}

Perrier, C. ^{[3
]}

Queloz, D. ^{[6
]}

Santerne, A. ^{[4
]}

Santos, N. C. ^{[5
,7
]}

Segransan, D. ^{[6
]}

Udry, S. ^{[6
]}

Vidal-Madjar, A. ^{[1
]}

机构：

[1] Univ Paris 06, CNRS, Inst Astrophys Paris, UMR7095, F-75014 Paris, France

[2] Observ Haute Provence, CNRS, OAMP, F-04870 St Michel, France

[3] UJF Grenoble 1, CNRS, INSU, IPAG,UMR 5274, F-38041 Grenoble, France

[4] Univ Aix Marseille 1, Lab Astrophys Marseille, CNRS, UMR6110, F-13388 Marseille, France

[5] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal

[6] Univ Geneva, Observ Geneva, CH-1290 Sauverny, Switzerland

[7] Univ Porto, Fac Ciencias, Dept Fis & Astron, P-4150762 Oporto, Portugal

来源：

ASTRONOMY & ASTROPHYSICS | 2011年 / 527卷

基金：

欧洲研究理事会; 瑞士国家科学基金会;

关键词：

planets and satellites: dynamical evolution and stability; techniques: radial velocities; planetary systems; stars: individual: HAT-P-6; EXTRA-SOLAR PLANETS; VELOCITY; ROTATION; TRANSIT; MISALIGNMENT; MIGRATION; COMPANION; SEARCH;

D O I：

10.1051/0004-6361/201016331

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We observed the transit of the HAT-P-6b exoplanet across its host star with the SOPHIE spectrograph (OHP, France). The resulting stellar radial velocities display the Rossiter-McLaughlin anomaly and reveal a retrograde orbit: the planetary orbital spin and the stellar rotational spin point in approximately opposite directions. A fit to the anomaly measures a sky-projected angle lambda = 166 degrees +/- 10 degrees between these two spin axes. All seven known retrograde planets are hot Jupiters with masses M-p < 3 M-Jup. About two thirds of the planets in this mass range, however, are prograde and aligned (lambda similar or equal to 0 degrees). In contrast, most of the more massive planets (M-p > 4 M-Jup) are prograde but misaligned. Different mechanisms may therefore be responsible for planetary obliquities above and below similar to 3.5 M-Jup.

引用

页数：4

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