0576950 - ASÚ 2024 RIV FR eng J - Článek v odborném periodiku
Deeg, H. J. - Georgieva, I. - Nowak, G. - Kabáth, Petr … celkem 52 autorů
TOI-1416: A system with a super-Earth planet with a 1.07 d period.
Astronomy & Astrophysics. Roč. 677, September (2023), č. článku A12. ISSN 0004-6361. E-ISSN 1432-0746
Institucionální podpora: RVO:67985815
Klíčová slova: planets and satellites * detection * terrestrial planets
Obor OECD: Astronomy (including astrophysics,space science)
Impakt faktor: 5.4, rok: 2023 ; AIS: 1.803, rok: 2023
Způsob publikování: Open access
DOI: https://doi.org/10.1051/0004-6361/202346370

TOI-1416 (BD+42 2504, HIP 70705) is a V = 10 late G- or early K-type dwarf star. TESS detected transits in its Sectors 16, 23, and 50 with a depth of about 455 ppm and a period of 1.07 days. Radial velocities (RVs) confirm the presence of the transiting planet TOI1416 b, which has a mass of 3.48 +/- 0.47 M-circle plus and a radius of 1.62 +/- 0.08 R-circle plus, implying a slightly sub-Earth density of 4.50(-0.83)(+0.99) g cm(-3). The RV data also further indicate a tentative planet, c, with a period of 27.4 or 29.5 days, whose nature cannot be verified due to strong suspicions of contamination by a signal related to the Moon's synodic period of 29.53 days. The nearly ultra-short-period planet TOI-1416 b is a typical representative of a short-period and hot (T-eq approximate to 1570 K) super-Earth-like planet. A planet model of an interior of molten magma containing a significant fraction of dissolved water provides a plausible explanation for its composition, and its atmosphere could be suitable for transmission spectroscopy with JWST. The position of TOI-1416 b within the radius-period distribution corroborates the idea that planets with periods of less than one day do not form any special group. It instead implies that ultra-short-period planets belong to a continuous distribution of super-Earth-like planets with periods ranging from the shortest known ones up to approximate to 30 days, their period-radius distribution is delimited against larger radii by the Neptune Desert and by the period-radius valley that separates super-Earths from sub-Neptune planets. In the abundance of small, short-periodic planets, a notable plateau has emerged between periods of 0.6-1.4 days, which is compatible with the low-eccentricity formation channel. For the Neptune Desert, its lower limits required a revision due to the increasing population of short-period planets, for periods shorter then 2 days, we establish a radius of 1.6 R-circle plus and a mass of 0.028 M-jup (corresponding to 8.9 M-circle plus) as the desert's lower limits. We also provide corresponding limits to the Neptune Desert against the planets' insolation and effective temperatures.
Trvalý link: https://hdl.handle.net/11104/0347225