Fridlund, M, Livingston, J, Gandolfi, D, Persson, CM, Lam, KWF, Stassun, KG, Hellier, C ORCID: https://orcid.org/0000-0002-3439-1439, Korth, J, Hatzes, AP, Malavolta, L, Luque, R, Redfield, S, Guenther, EW, Albrecht, S, Barragan, O, Benatti, S, Bouma, L, Cabrera, J, Cochran, WD, Csizmadia, S, Dai, F, Deeg, HJ, Esposito, M, Georgieva, I, Grziwa, S, Cuesta, LG, Hirano, T, Jenkins, JM, Kabath, P, Knudstrup, E, Latham, DW, Mathur, S, Mullally, SE, Narita, N, Nowak, G, Olofsson, AOH, Palle, E, Pätzold, M, Pompei, E, Rauer, H, Ricker, G, Rodler, F, Seager, S, Serrano, LM, Smith, AMS, Spina, L, Subjak, J, Tenenbaum, P, Ting, EB, Vanderburg, A, Vanderspek, R, Van Eylen, V, Villanueva, S and Winn, JN (2020) The TOI-763 system: sub-Neptunes orbiting a Sun-like star. Monthly Notices of the Royal Astronomical Society.

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Abstract

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 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 radial velocity data. The inner transiting planet, TOI-763 b, has an orbital period of Pb = 5.6 days, 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 days, 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 days. 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.

Item Type: Article
Additional Information: © 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model)
Uncontrolled Keywords: Planets and satellites: detection, Planets and satellites: individual: (TOI-763, TIC 178819686)
Subjects: Q Science > QB Astronomy
Q Science > QB Astronomy > QB460 Astrophysics
Q Science > QB Astronomy > QB600 Planets. Planetology
Q Science > QC Physics
Divisions: Faculty of Natural Sciences > School of Chemical and Physical Sciences
Depositing User: Symplectic
Date Deposited: 10 Sep 2020 09:43
Last Modified: 10 Sep 2020 09:43
URI: https://eprints.keele.ac.uk/id/eprint/8644

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