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The TOI-763 system: sub-Neptunes orbiting a Sun-like star

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DOI

  • M. Fridlund, Leiden University, Chalmers University of Technology
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  • J. Livingston, University of Tokyo
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  • D. Gandolfi, Universita di Torino
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  • C. M. Persson, Chalmers University of Technology
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  • K. W.F. Lam, Technical University of Berlin
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  • K. G. Stassun, Vanderbilt University
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  • C. Hellier, Keele University
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  • J. Korth, University of Cologne
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  • A. P. Hatzes, Thüringer Landessternwarte Tautenburg
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  • L. Malavolta, University of Padova
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  • R. Luque, Instituto Astrofisico de Canarias, University of La Laguna
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  • S. Redfield, Wesleyan University
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  • E. W. Guenther, Thüringer Landessternwarte Tautenburg
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  • S. Albrecht
  • O. Barragan, University of Oxford
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  • S. Benatti, University of Palermo
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  • L. Bouma, Princeton University
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  • J. Cabrera, German Aerospace Center
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  • W. D. Cochran, University of Texas at Austin
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  • S. Csizmadia, German Aerospace Center
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  • F. Dai, Princeton University, Massachusetts Institute of Technology
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  • H. J. Deeg, Instituto Astrofisico de Canarias, University of La Laguna
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  • M. Esposito, Thüringer Landessternwarte Tautenburg
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  • I. Georgieva, Chalmers University of Technology
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  • S. Grziwa, University of Cologne
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  • L. González Cuesta, Instituto Astrofisico de Canarias, University of La Laguna
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  • T. Hirano, Tokyo Institute of Technology
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  • J. M. Jenkins, NASA Ames Research Center
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  • P. Kabath, Czech Academy of Sciences
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  • E. Knudstrup
  • D. W. Latham, Harvard-Smithsonian Center for Astrophysics
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  • S. Mathur, Instituto Astrofisico de Canarias, University of La Laguna
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  • S. E. Mullally, Massachusetts Institute of Technology
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  • N. Narita, Instituto Astrofisico de Canarias, National Institutes of Natural Sciences - National Astronomical Observatory of Japan, University of Tokyo, Japan Science and Technology Agency, NINS
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  • G. Nowak, Instituto Astrofisico de Canarias, University of La Laguna
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  • A. O.H. Olofsson, Chalmers University of Technology
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  • E. Palle, Instituto Astrofisico de Canarias, University of La Laguna
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  • M. Pätzold, University of Cologne
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  • E. Pompei, European Southern Observatory
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  • H. Rauer, Technical University of Berlin, German Aerospace Center, Free University of Berlin
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  • G. Ricker, Massachusetts Institute of Technology
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  • F. Rodler, European Southern Observatory
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  • S. Seager, Massachusetts Institute of Technology
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  • L. M. Serrano, Universita di Torino
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  • A. M.S. Smith, German Aerospace Center
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  • L. Spina, Monash University, ARC Centre of Excellence for All Sky Astrophysics in Three Dimensions (ASTRO-3D)
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  • J. Subjak, Czech Academy of Sciences, Charles University
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  • P. Tenenbaum, NASA Ames Research Center
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  • E. B. Ting, NASA Ames Research Center
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  • A. Vanderburg, University of Wisconsin-Madison
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  • R. Vanderspek, Massachusetts Institute of Technology
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  • V. Van Eylen, University College London
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  • S. Villanueva, Massachusetts Institute of Technology
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  • J. N. Winn, Princeton University

We report the discovery of a planetary system orbiting TOI-763(aka CD-39 7945), a V = 10.2, high proper motion G-type dwarf star that was photometrically monitored by the TESS space mission in Sector 10. We obtain and model the stellar spectrum and find an object slightly smaller than the Sun, and somewhat older, but with a similar metallicity. Two planet candidates were found in the light curve to be transiting the star. Combining TESS transit photometry with HARPS high-precision radial velocity (RV) follow-up measurements confirm the planetary nature of these transit signals. We determine masses, radii, and bulk densities of these two planets. A third planet candidate was discovered serendipitously in the RV data. The inner transiting planet, TOI-763 b, has an orbital period of Pb = 5.6 d, a mass of Mb = 9.8 ± 0.8 M⊕, and a radius of Rb = 2.37 ± 0.10 R⊕. The second transiting planet, TOI-763 c, has an orbital period of Pc = 12.3 d, a mass of Mc = 9.3 ± 1.0 M⊕, and a radius of Rc = 2.87 ± 0.11 R⊕. We find the outermost planet candidate to orbit the star with a period of ∼48 d. If confirmed as a planet, it would have a minimum mass of Md = 9.5 ± 1.6 M⊕. We investigated the TESS light curve in order to search for a mono transit by planet d without success. We discuss the importance and implications of this planetary system in terms of the geometrical arrangements of planets orbiting G-type stars.

OriginalsprogEngelsk
TidsskriftMonthly Notices of the Royal Astronomical Society
Vol/bind498
Nummer3
Sider (fra-til)4503-4517
Antal sider15
ISSN0035-8711
DOI
StatusUdgivet - nov. 2020

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