Статья

OBLIQUITIES OF HOT JUPITER HOST STARS: EVIDENCE FOR TIDAL INTERACTIONS AND PRIMORDIAL MISALIGNMENTS

Simon AlbrechtDepartment of Physics and Kavli Institute for Astrophysics & Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USAJoshua N. WinnDepartment of Physics and Kavli Institute for Astrophysics & Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USAJohn Asher JohnsonDepartment of Astrophysics, California Institute of Technology, MC249-17, Pasadena, CA 91125, USAAndrew W. HowardDepartment of Astronomy,University of California,Berkeley,CA 94720,USAGeoffrey W. MarcyDepartment of Astronomy,University of California,Berkeley,CA 94720,USAR. Paul ButlerDepartment of Terrestrial Magnetism, Carnegie Institution of Washington, 5241 Broad Branch Road, NW Washington DC, 20015, USAP. ArriagadaDept. of Astronomy, Pontificia Universidad Católica de Chile, Casilla 306, Santiago 22, ChileJeffrey D. CraneThe Observatories of the Carnegie Institution of Washington, 813 Santa Barbara Street, Pasadena, CA 91101, USA,Stephen A. ShectmanThe Observatories of the Carnegie Institution of Washington, 813 Santa Barbara Street, Pasadena, CA 91101, USA,Ian B. ThompsonThe Observatories of the Carnegie Institution of Washington, 813 Santa Barbara Street, Pasadena, CA 91101, USA,Teruyuki HiranoDepartment of Physics, the University of Tokyo, Tokyo 113-0033, JapanG. Á. BakosAlfred. P. Sloan FellowJ. D. HartmanDepartment of Astrophysical Sciences, Princeton University, Peyton Hall, Princeton NJ 08544, USA

2012en

ABI

Аннотация

We provide evidence that the obliquities of stars with close-in giant planets were initially nearly random, and that the low obliquities that are often observed are a consequence of star-planet tidal interactions. The evidence is based on 14 new measurements of the Rossiter-McLaughlin effect (for the systems HAT-P-6, HAT-P-7, HAT-P-16, HAT-P-24, HAT-P-32, HAT-P-34, WASP-12, WASP-16, WASP-18, WASP-19, WASP-26, WASP-31, Gl 436, and Kepler-8), as well as a critical review of previous observations. The low-obliquity (well-aligned) systems are those for which the expected tidal timescale is short, and likewise the high-obliquity (misaligned and retrograde) systems are those for which the expected timescale is long. At face value, this finding indicates that the origin of hot Jupiters involves dynamical interactions like planet-planet interactions or the Kozai effect that tilt their orbits rather than inspiraling due to interaction with a protoplanetary disk. We discuss the status of this hypothesis and the observations that are needed for a more definitive conclusion.

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Идентификаторы

DOI: 10.1088/0004-637x/757/1/18

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Цитирований: 3Использованных источников: 0

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