TOI−757 b: an eccentric transiting mini−Neptune on a 17.5−d orbit
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| Název: | TOI−757 b: an eccentric transiting mini−Neptune on a 17.5−d orbit |
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| Autoři: | Alqasim, A., Grieves, N., Rosário, N. M., Gandolfi, D., Livingston, J.H., Sousa, S.G., Collins, Karen A., Teske, J. K., Fridlund, Malcolm, 1952, Egger, J. A., Cabrera, J., Hellier, Coel, Lanza, A. F., Van Eylen, Vincent, Bouchy, F., Oelkers, R.J., Srdoc, G., Wilson, T.G., Goffo, E., Delrez, L., Sefako, Ramotholo, Barros, S.C.C., Collins, Kevin I., Heitzmann, A., Bonfanti, A., Bárczy, T., Barrado Navascues, D., Billot, N., Borsato, L., Broeg, C., Alonso, R., Asquier, J., Baumjohann, W., Benz, W., Bryant, E., Butler, R.P., Collier Cameron, A., Correia, A., Crane, J.D., Cubillos, P. E., Davies, M. B., Deline, A., Demory, B.O., Deleuil, M., Cochran, William D., Csizmadia, Szilard, Derekas, A., Edwards, Billy, Daylan, Tansu, Erikson, Anders, Gazeas, K., Gudel, M., Hasiba, J., Hatzes, A., Helling, Ch., Hirano, T., Jenkins, Jon M., Kanodia, S., Kiss, L. L., Laskar, J., des Etangs, A. L., Lendl, M., Lund, M. B., Luque, R., Mann, A., Magrin, D., Maxted, P., Mordasini, C., Fortier, A., Olofsson, G., Ehrenreich, D., Pagano, I., Nascimbeni, Valerio, Osborn, H. P., Rando, N., Ottensamer, R., Isaak, K., Korth, Judith, 1987, Gillon, Michaël, Peter, G., Piotto, Giampaolo P., Hoyer, S., Howell, S.B., Rieder, M., Palle, E., Essack, Zahra, Lam, K. W.F., Ragazzoni, Roberto, Rauer, H., Redfield, S., Ribas, I., Segransan, D., Ricker, George R., Santos, N. C., Scandariato, Gaetano, Stalport, M., Shporer, Avi, Simon, A.E., Smith, Alexis M. S., Szabó, G.M., Twicken, J. D., Udry, S., Vanderspek, Roland K., Van Grootel, V., Venturini, J., Viotto, V., Walton, N. A., Winn, J. N., Yee, S.W. |
| Zdroj: | Monthly Notices of the Royal Astronomical Society. 533(1):1-26 |
| Témata: | planets and satellites: composition, planets and satellites: interiors, techniques: photometric, techniques: radial velocities, stars: individual: TOI-757 (TIC 130924120) |
| Popis: | We report the spectroscopic confirmation and fundamental properties of TOI−757 b, a mini−Neptune on a 17.5−d orbit transiting a bright star (V = 9.7 mag) discovered by the TESS mission. We acquired high−precision radial velocity measurements with the HARPS, ESPRESSO, and PFS spectrographs to confirm the planet detection and determine its mass. We also acquired space−borne transit photometry with the CHEOPS space telescope to place stronger constraints on the planet radius, supported with ground−based LCOGT photometry. WASP and KELT photometry were used to help constrain the stellar rotation period. We also determined the fundamental parameters of the host star. We find that TOI−757 b has a radius of Rp = 2.5 ± 0.1R. and a mass of Mp = 10.5+−2212M, implying a bulk density of ρp = 3.6 ± 0.8 g cm−3. Our internal composition modelling was unable to constrain the composition of TOI−757 b, highlighting the importance of atmospheric observations for the system. We also find the planet to be highly eccentric with e = 0.39+−000708, making it one of the very few highly eccentric planets among precisely characterized mini−Neptunes. Based on comparisons to other similar eccentric systems, we find a likely scenario for TOI−757 b’s formation to be high eccentricity migration due to a distant outer companion. We additionally propose the possibility of a more intrinsic explanation for the high eccentricity due to star−star interactions during the earlier epoch of the Galactic disc formation, given the low metallicity and older age of TOI−757. |
| Popis souboru: | electronic |
| Přístupová URL adresa: | https://research.chalmers.se/publication/542403 https://research.chalmers.se/publication/542403/file/542403_Fulltext.pdf |
| Databáze: | SwePub |
Nájsť tento článok vo Web of Science | Abstrakt: | We report the spectroscopic confirmation and fundamental properties of TOI−757 b, a mini−Neptune on a 17.5−d orbit transiting a bright star (V = 9.7 mag) discovered by the TESS mission. We acquired high−precision radial velocity measurements with the HARPS, ESPRESSO, and PFS spectrographs to confirm the planet detection and determine its mass. We also acquired space−borne transit photometry with the CHEOPS space telescope to place stronger constraints on the planet radius, supported with ground−based LCOGT photometry. WASP and KELT photometry were used to help constrain the stellar rotation period. We also determined the fundamental parameters of the host star. We find that TOI−757 b has a radius of Rp = 2.5 ± 0.1R. and a mass of Mp = 10.5+−2212M, implying a bulk density of ρp = 3.6 ± 0.8 g cm−3. Our internal composition modelling was unable to constrain the composition of TOI−757 b, highlighting the importance of atmospheric observations for the system. We also find the planet to be highly eccentric with e = 0.39+−000708, making it one of the very few highly eccentric planets among precisely characterized mini−Neptunes. Based on comparisons to other similar eccentric systems, we find a likely scenario for TOI−757 b’s formation to be high eccentricity migration due to a distant outer companion. We additionally propose the possibility of a more intrinsic explanation for the high eccentricity due to star−star interactions during the earlier epoch of the Galactic disc formation, given the low metallicity and older age of TOI−757. |
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| ISSN: | 00358711 13652966 |
| DOI: | 10.1093/mnras/stae1767 |