The Aligned Orbit of the Eccentric Warm Jupiter K2-232b

被引：22

作者：

Wang, Songhu ^{[1
]}

Winn, Joshua N. ^{[2
]}

Addison, Brett C. ^{[3
]}

Dai, Fei ^{[4
]}

Rice, Malena ^{[5
]}

Holden, Bradford ^{[6
]}

Burt, Jennifer A. ^{[7
]}

Wang, Xian-Yu ^{[8
,9
]}

Butler, R. Paul ^{[10
]}

Vogt, Steven S.

Laughlin, Gregory ^{[5
]}

机构：

[1] Indiana Univ, Dept Astron, Bloomington, IN 47405 USA

[2] Princeton Univ, Dept Astrophys Sci, 4 Ivy Lane, Princeton, NJ 08544 USA

[3] Univ Southern Queensland, Ctr Astrophys, West St, Toowoomba, Qld 4350, Australia

[4] Div Geol & Planetary Sci, 1200 E Calif Blvd, Pasadena, CA 91125 USA

[5] Yale Univ, Dept Astron, New Haven, CT 06511 USA

[6] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA

[7] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA

[8] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China

[9] Univ Chinese Acad Sci, Beijing 100049, Peoples R China

[10] Carnegie Inst Sci, Earth & Planets Lab, 5241 Broad Branch Rd NW, Washington, DC 20015 USA

来源：

ASTRONOMICAL JOURNAL | 2021年 / 162卷 / 02期

基金：

美国国家航空航天局; 美国国家科学基金会;

关键词：

EXTRASOLAR PLANETS; SPIN; STAR; BINARY; RETROGRADE; ALIGNMENT; EVOLUTION; ROTATION;

D O I：

10.3847/1538-3881/ac0626

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Measuring the obliquity distribution of stars hosting warm Jupiters may help us to understand the formation of close-orbiting gas giants. Few such measurements have been performed due to practical difficulties in scheduling observations of the relatively infrequent and long-duration transits of warm Jupiters. Here, we report a measurement of the Rossiter-McLaughlin effect for K2-232 b, a warm Jupiter on an 11.17 day orbit with an eccentricity of 0.26. The data were obtained with the Automated Planet Finder during two separate transits. The planet's orbit appears to be well aligned with the spin axis of the host star, with a projected spin-orbit angle of lambda = -11.degrees 1 +/- 6.degrees 6. Combined with the other available data, we find that high obliquities are almost exclusively associated with planets that either have an orbital separation greater than 10 stellar radii or orbit stars with effective temperatures hotter than 6000 K. This pattern suggests that the obliquities of the closest-orbiting giant planets around cooler stars have been damped by tidal effects.

引用

页数：6

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