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TOI-220b: a warm sub-Neptune discovered by TESS

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Titel: TOI-220b: a warm sub-Neptune discovered by TESS
Autoren: Hoyer, S., Gandolfi, D., Armstrong, D. J., Deleuil, M., Acuna, L., de Medeiros, J. R., Goffo, E., Lillo-Box, J., Delgado Mena, E., Lopez, T. A., Santerne, A., Sousa, S., Fridlund, Malcolm, 1952, Adibekyan, V, Collins, K. A., Serrano, L. M., Cortes-Zuleta, P., Howell, S. B., Deeg, H., Aguichine, A., Barragan, O., Bryant, E. M., Canto Martins, B. L., Collins, Cooke, B. F., Diaz, R. F., Esposito, M., Furlan, E., Hojjatpanah, S., Jackman, J., Jenkins, J. M., Jensen, E. L. N., Latham, D. W., Leao, I. C., Matson, R. A., Nielsen, L. D., Osborn, A., Otegi, J. F., Rodler, F., Sabotta, S., Scott, N. J., Seager, S., Stockdale, C., Strom, 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., Kabath, P., Knudstrup, E., Korth, Judith, 1987, Livingston, J. H., Luque, R., Mousis, O., Mullally, S. E., Osborn, H. P., Palle, E., Persson, Carina, 1964, Redfield, S., Santos, N. C., Smith, J., Subjak, J., Twicken, J. D., Udry, S., Yahalomi, D. A.
Quelle: Monthly Notices of the Royal Astronomical Society. 505(3):3361-3379
Schlagwörter: techniques: radial velocities, planets and satellites: fundamental parameters, techniques: photometric, stars: fundamental parameters, planets and satellites: individual: TYC 8897-01263-1
Beschreibung: In this paper, we report the discovery of TOI-220b, 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 +/- 1.0M(circle plus) and radius of 3.03 +/- 0.15R(circle plus), implying a bulk density of 2.73 +/- 0.47. TOI-220b orbits a relative bright (V=10.4) and old (10.1 +/- 1.4Gyr) K dwarf star with a period of similar to 10.69d. Thus, TOI-220b is a new warm sub-Neptune with very precise mass and radius determinations. A Bayesian analysis of the TOI-220b 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.
Dateibeschreibung: electronic
Zugangs-URL: https://research.chalmers.se/publication/525341
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  Data: <i>Monthly Notices of the Royal Astronomical Society</i>. 505(3):3361-3379
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  Data: <searchLink fieldCode="DE" term="%22techniques%3A+radial+velocities%22">techniques: radial velocities</searchLink><br /><searchLink fieldCode="DE" term="%22planets+and+satellites%3A+fundamental+parameters%22">planets and satellites: fundamental parameters</searchLink><br /><searchLink fieldCode="DE" term="%22techniques%3A+photometric%22">techniques: photometric</searchLink><br /><searchLink fieldCode="DE" term="%22stars%3A+fundamental+parameters%22">stars: fundamental parameters</searchLink><br /><searchLink fieldCode="DE" term="%22planets+and+satellites%3A+individual%3A+TYC+8897-01263-1%22">planets and satellites: individual: TYC 8897-01263-1</searchLink>
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  Data: In this paper, we report the discovery of TOI-220b, 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 +/- 1.0M(circle plus) and radius of 3.03 +/- 0.15R(circle plus), implying a bulk density of 2.73 +/- 0.47. TOI-220b orbits a relative bright (V=10.4) and old (10.1 +/- 1.4Gyr) K dwarf star with a period of similar to 10.69d. Thus, TOI-220b is a new warm sub-Neptune with very precise mass and radius determinations. A Bayesian analysis of the TOI-220b 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.
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              M: 01
              Type: published
              Y: 2021
          Identifiers:
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              Value: 00358711
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            – Type: issue
              Value: 3
          Titles:
            – TitleFull: Monthly Notices of the Royal Astronomical Society
              Type: main
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