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TOI-1416: A system with a super-Earth planet with a 1.07 d period
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SYSNO ASEP 0576950 Druh ASEP J - Článek v odborném periodiku Zařazení RIV J - Článek v odborném periodiku Poddruh J Článek ve WOS Název TOI-1416: A system with a super-Earth planet with a 1.07 d period Tvůrce(i) Deeg, H. J. (ES)
Georgieva, I. (SE)
Nowak, G. (ES)
Kabáth, Petr (ASU-R) ORCIDCelkový počet autorů 52 Číslo článku A12 Zdroj.dok. Astronomy & Astrophysics. - : EDP Sciences - ISSN 0004-6361
Roč. 677, September (2023)Poč.str. 29 s. Forma vydání Online - E Jazyk dok. eng - angličtina Země vyd. FR - Francie Klíč. slova planets and satellites ; detection ; terrestrial planets Obor OECD Astronomy (including astrophysics,space science) Způsob publikování Open access Institucionální podpora ASU-R - RVO:67985815 UT WOS 001063425400004 EID SCOPUS 85170822852 DOI https://doi.org/10.1051/0004-6361/202346370 Anotace 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. Pracoviště Astronomický ústav Kontakt Anežka Melichárková, bibl@asu.cas.cz, Tel.: 323 620 326 Rok sběru 2024 Elektronická adresa https://hdl.handle.net/11104/0347225
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