Статья

Obliquities of exoplanet host stars

E. KnudstrupDepartment of Space, Earth and Environment, Chalmers University of Technology, 412 93 Gothenburg, SwedenS. H. AlbrechtDepartment of Astrophysical Sciences, Princeton University, 4 Ivy Lane, Princeton, NJ 08544, USAJ. N. WinnDepartment of Astrophysical Sciences, Princeton University, 4 Ivy Lane, Princeton, NJ 08544, USAD. GandolfiDipartimento di Fisica, Universita degli Studi di Torino, via Pietro Giuria 1, 10125 Torino, ItalyJ. J. ZanazziAstronomy Department, Theoretical Astrophysics Center, and Center for Integrative Planetary Science, University of California, Berkeley, Berkeley, CA 94720, USAC. M. PerssonChalmers University of Technology, Department of Space, Earth and Environment, Onsala Space Observatory, 439 92 Onsala, SwedenM. FridlundChalmers University of Technology, Department of Space, Earth and Environment, Onsala Space Observatory, 439 92 Onsala, SwedenMarcus L. MarcussenStellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, 8000 Aarhus C, DenmarkA. ChontosDepartment of Astrophysical Sciences, Princeton University, 4 Ivy Lane, Princeton, NJ 08544, USAMarcelo Aron Fetzner KenigerDepartment of Physics, University of Warwick, Gibbet Hill Road, Coventry CV4 7AL, UKNora L. EisnerCenter for Computational Astrophysics, Flatiron Institute, 162 Fifth Avenue, New York, NY 10010, USAAllyson BierylaCenter for Astrophysics | Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138, USAH. Isaacson501 Campbell Hall, University of California at Berkeley, Berkeley, CA 94720, USAA.W. HowardDepartment of Astronomy, California Institute of Technology, Pasadena, CA 91125, USAL. A. HirschDepartment of Chemical and Physical Sciences, University of Toronto Mississauga, Mississauga, ON, CanadaF. MurgasDepartamento de Astrofísica, Universidad de La Laguna (ULL), 38206 La Laguna, Tenerife, SpainN. NaritaAstrobiology Center, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, JapanE. PalleDepartamento de Astrofísica, Universidad de La Laguna (ULL), 38206 La Laguna, Tenerife, SpainY. KawaiDepartment of Multi-Disciplinary Sciences, Graduate School of Arts and Sciences, The University of Tokyo, 3-8-1 Komaba, Meguro, Tokyo 153-8902, JapanD. BakerPhysics Department, Austin College, Sherman, TX 75090, USA

2024en

ABI

Аннотация

Measurements of the obliquities in exoplanet systems have revealed some remarkable architectures, some of which are very different from the Solar System. Nearly 200 obliquity measurements have been obtained through observations of the Rossiter–McLaughlin (RM) effect. Here, we report on observations of 19 planetary systems that led to 17 clear detections of the RM effect and 2 less secure detections. After adding the new measurements to the tally, we used the entire collection of RM measurements to investigate four issues that have arisen in the literature. i) Does the obliquity distribution show a peak at approximately 90°? We find tentative evidence that such a peak does exist when restricting attention to the sample of sub-Saturn planets and hot Jupiters orbiting F stars. ii) Are high obliquities associated with high eccentricities? We find the association to be weaker than previously reported, and that a stronger association exists between obliquity and orbital separation, possibly due to tidal obliquity damping at small separations. iii) How low are the lowest known obliquities? Among hot Jupiters around cool stars, we find the dispersion to be 1.4 ± 0.7°, smaller than the 6° obliquity of the Sun, which serves as additional evidence for tidal damping. iv) What are the obliquities of stars with compact and flat systems of multiple planets? We find that they generally have obliquities lower than 10°, with several remarkable exceptions possibly caused by wide-orbiting stellar or planetary companions.

Перевод пока недоступен

Идентификаторы

DOI: 10.1051/0004-6361/202450627

Цитирования и источники

Цитирований: 3Использованных источников: 0

Показатели — AkademScholar