학술논문
TOI-220 $b$: a warm sub-Neptune discovered by TESS
Document Type
Working Paper
Author
Hoyer, S.; Gandolfi, D.; Armstrong, D. J.; Deleuil, M.; Acuña, L.; de Medeiros, J. R.; Goffo, E.; Lillo-Box, J.; Mena, E. Delgado; Lopez, T. A.; Santerne, A.; Sousa, S.; Fridlund, M.; Adibekyan, V.; Collins, K. A.; Serrano, L. M.; Cortés-Zuleta, P.; Howell, S. B.; Deeg, H.; Aguichine, A.; Barragán, O.; Bryant, E. M.; Martins, B. L. Canto; Collins, K. I.; Cooke, B. F.; Díaz, R. F.; Esposito, M.; Furlan, E.; Hojjatpanah, S.; Jackman, J.; Jenkins, J. M.; Jensen, E. L. N.; Latham, D. W.; Leão, I. C.; Matson, R. A.; Nielsen, L. D.; Osborn, A.; Otegi, J. F.; Rodler, F.; Sabotta, S.; Scott, N. J.; Seager, S.; Stockdale, C.; Strøm, P. A.; Vanderspek, R.; Van Eylen, V.; Wheatley, P. J.; Winn, J. N.; Almenara, J. M.; Barrado, D.; Barros, S. C. C.; Bayliss, D.; Bouchy, F.; Boyd, P. T.; Cabrera, J.; Cochran, W. D.; Demangeon, O.; Doty, J. P.; Dumusque, X.; Figueira, P.; Fong, W.; Grziwa, S.; Hatzes, A. P.; Kabáth, P.; Knudstrup, E.; Korth, J.; Livingston, J. H.; Luque, R.; Mousis, O.; Mullally, S. E.; Osborn, H. P.; Pallé, E.; Persson, C. M.; Redfield, S.; Santos, N. C.; Smith, J.; Šubjak, J.; Twicken, J. D.; Udry, S.; Yahalomi, D. A.
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Subject
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Abstract
In this paper we report the discovery of TOI-220 $b$, a new sub-Neptune detected by the Transiting Exoplanet Survey Satellite (TESS) and confirmed by radial velocity follow-up observations with the HARPS spectrograph. Based on the combined analysis of TESS transit photometry and high precision radial velocity measurements we estimate a planetary mass of 13.8 $\pm$ 1.0 M$_{Earth}$ and radius of 3.03 $\pm$ 0.15 R$_{Earth}$, implying a bulk density of 2.73 $\pm$ 0.47 $\textrm{g cm}^{-3}$. TOI-220 $b$ orbits a relative bright (V=10.4) and old (10.1$\pm$1.4 Gyr) K dwarf star with a period of $\sim$10.69 d. Thus, TOI-220 $b$ is a new warm sub-Neptune with very precise mass and radius determinations. A Bayesian analysis of the TOI-220 $b$ internal structure indicates that due to the strong irradiation it receives, the low density of this planet could be explained with a steam atmosphere in radiative-convective equilibrium and a supercritical water layer on top of a differentiated interior made of a silicate mantle and a small iron core.
Comment: Accepted for publication in MNRAS
Comment: Accepted for publication in MNRAS