The TOI-763 system: sub-Neptunes orbiting a Sun-like star
| Autor: | Enric Palle, Jon M. Jenkins, Vincent Van Eylen, Seth Redfield, Coel Hellier, Simon Albrecht, Oscar Barragán, Martin Pätzold, William D. Cochran, Emanuela Pompei, Roland Vanderspek, Judith Korth, George R. Ricker, Norio Narita, L. M. Serrano, John H. Livingston, Sascha Grziwa, Eike W. Guenther, Fei Dai, S. E. Mullally, S. Villanueva, Eric B. Ting, K. W. F. Lam, Andrew Vanderburg, Rafael Luque, Alexis M. S. Smith, Carina M. Persson, M. Esposito, Teriyuki Hirano, Malcolm Fridlund, P. Tenenbaum, Hans J. Deeg, Florian Rodler, Joshua N. Winn, Serena Benatti, Davide Gandolfi, Szilard Csizmadia, Luke G. Bouma, Emil Knudstrup, Lorenzo Spina, A. P. Hatzes, J. Cabrera, Savita Mathur, Grzegorz Nowak, Keivan G. Stassun, David W. Latham, Sara Seager, Luca Malavolta, Heike Rauer, L. González Cuesta, Jan Subjak, A. O. H. Olofsson, Petr Kabath, Iskra Georgieva |
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| Jazyk: | angličtina |
| Rok vydání: | 2020 |
| Předmět: |
Extrasolare Planeten und Atmosphären
planets and satellites: individual: TIC 178819686 Dwarf star planets and satellites: detection Proper motion detection [planets and satellites] Metallicity planets and satellites: individual: TOI-763 FOS: Physical sciences Astrophysics::Cosmology and Extragalactic Astrophysics 01 natural sciences 010309 optics individual: TIC 178819686 [planets and satellites] Planet QB460 0103 physical sciences 010303 astronomy & astrophysics QB600 QC individual: TOI-763 [planets and satellites] QB Physics Earth and Planetary Astrophysics (astro-ph.EP) Leitungsbereich PF Astronomy Astronomy and Astrophysics Planetary system Orbital period Light curve Radial velocity 13. Climate action Space and Planetary Science Astrophysics::Earth and Planetary Astrophysics Astrophysics - Earth and Planetary Astrophysics |
| Zdroj: | arXiv Fridlund, M, Livingston, J, Gandolfi, D, Persson, C M, Lam, K W F, Stassun, K G, Hellier, C, Korth, J, Hatzes, A P, Malavolta, L, Luque, R, Redfield, S, Guenther, E W, Albrecht, S, Barragan, O, Benatti, S, Bouma, L, Cabrera, J, Cochran, W D, Csizmadia, S, Dai, F, Deeg, H J, Esposito, M, Georgieva, I, Grziwa, S, González Cuesta, L, Hirano, T, Jenkins, J M, Kabath, P, Knudstrup, E, Latham, D W, Mathur, S, Mullally, S E, Narita, N, Nowak, G, Olofsson, A O H, Palle, E, Pätzold, M, Pompei, E, Rauer, H, Ricker, G, Rodler, F, Seager, S, Serrano, L M, Smith, A M S, Spina, L, Subjak, J, Tenenbaum, P, Ting, E B, Vanderburg, A, Vanderspek, R, Van Eylen, V, Villanueva, S & Winn, J N 2020, ' The TOI-763 system : sub-Neptunes orbiting a Sun-like star ', Monthly Notices of the Royal Astronomical Society, vol. 498, no. 3, pp. 4503-4517 . https://doi.org/10.1093/mnras/staa2502 Monthly Notices of the Royal Astronomical Society Monthly Notices of the Royal Astronomical Society, 498(3), 4503-4517 |
| ISSN: | 0035-8711 |
| Popis: | 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 $P_\mathrm{b}$ = 5.6~days, a mass of $M_\mathrm{b}$ = $9.8\pm0.8$ $M_\oplus$, and a radius of $R_\mathrm{b}$ = $2.37\pm0.10$ $R_\oplus$. The second transiting planet,TOI-763 c, has an orbital period of $P_\mathrm{c}$ = 12.3~days, a mass of $M_\mathrm{c}$ = $9.3\pm1.0$ $M_\oplus$, and a radius of $R_\mathrm{c}$ = $2.87\pm0.11$ $R_\oplus$. We find the outermost planet candidate to orbit the star with a period of $\sim$48~days. If confirmed as a planet it would have a minimum mass of $M_\mathrm{d}$ = $9.5\pm1.6$ $M_\oplus$. 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. |
| Databáze: | OpenAIRE |
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