A HIGH STELLAR OBLIQUITY IN THE WASP-7 EXOPLANETARY SYSTEM

被引：43

作者：

Albrecht, Simon ^{[1
,2
]}

Winn, Joshua N. ^{[1
,2
]}

Butler, R. Paul ^{[3
]}

Crane, Jeffrey D. ^{[4
]}

Shectman, Stephen A. ^{[4
]}

Thompson, Ian B. ^{[4
]}

Hirano, Teruyuki ^{[1
,2
,5
]}

Wittenmyer, Robert A. ^{[6
]}

机构：

[1] MIT, Dept Phys, Cambridge, MA 02139 USA

[2] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA

[3] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA

[4] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA

[5] Univ Tokyo, Dept Phys, Tokyo 1130033, Japan

[6] Univ New S Wales, Sch Phys, Dept Astrophys, Sydney, NSW 2052, Australia

来源：

ASTROPHYSICAL JOURNAL | 2012年 / 744卷 / 02期

关键词：

planetary systems; planets and satellites: formation; planet-star interactions; stars: individual (WASP-7); stars: rotation; techniques: spectroscopic; TRANSITING EXOPLANETS; HOT JUPITERS; SPIN-ORBIT; ROTATION; PLANETS; CURVES; BINARY; STARS;

D O I：

10.1088/0004-637X/744/2/189

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We measure a tilt of 86 degrees +/- 6 degrees. between the sky projections of the rotation axis of the WASP-7 star and the orbital axis of its close-in giant planet. This measurement is based on observations of the Rossiter-McLaughlin (RM) effect with the Planet Finder Spectrograph on the Magellan II telescope. The result conforms with the previously noted pattern among hot-Jupiter hosts, namely, that the hosts lacking thick convective envelopes have high obliquities. Because the planet's trajectory crosses a wide range of stellar latitudes, observations of the RM effect can in principle reveal the stellar differential rotation profile; however, with the present data the signal of differential rotation could not be detected. The host star is found to exhibit radial-velocity noise ("stellar jitter") with an amplitude of approximate to 30 m s(-1) over a timescale of days.

引用

页数：9

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