TOI-1416: A system with a super-Earth planet with a 1.07d period

• Published in: arXiv.org
• Main Authors: Deeg, H J, Georgieva, I Y, Nowak, G, Persson, C M, Cale, B L, Murgas, F, Pallé, E, D Godoy Rivera, Dai, F, Ciardi, D R, Akana Murphy, J M, Beck, P G, Burke, C J, Cabrera, J, Carleo, I, Cochran, W D, Collins, K A, Csizmadia, Sz, M El Mufti, Fridlund, M, Fukui, A, Gandolfi, D, García, R A, Guenther, E W, Guerra, P, Grziwa, S, Isaacson, H, Isogai, K, Jenkins, J M, Kábath, P, Korth, J, Lam, K W F, Latham, D W, Luque, R, Lund, M B, Livingston, J H, Mathis, S, Mathur, S, Narita, N, Orell-Miquel, J, Osborne, H L M, Parviainen, H, Plavchan, P P, Redfield, S, Rodriguez, D R, Schwarz, R P, Seager, S, Smith, A M S, V Van Eylen, J Van Zandt, Winn, J N, Ziegler, C
• Format: Paper Journal Article
• Language: English
• Published: Ithaca Cornell University Library, arXiv.org 29.05.2023
• Subjects: Dwarf stars; Earth; Extrasolar planets; Magma; Physics - Earth and Planetary Astrophysics; Terrestrial planets; Transit
• ISSN: 2331-8422
• DOI: 10.48550/arxiv.2305.18542

TOI 1416 (BD+42 2504, HIP 70705) is a V=10 late G or early K-type dwarf star with transits detected by TESS. Radial velocities verify the presence of the transiting planet TOI-1416 b, with a period of 1.07d, a mass of \(3.48 M_{Earth}\) and a radius of \(1.62 R_{Earth}\), implying a slightly sub-Earth density of \(4.50\) 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 about contamination by a signal related to the Moon's synodic period of 29.53 days. The near-USP (Ultra Short Period) planet TOI-1416 b is a typical representative of a short-period and hot (\(T_{eq} \approx\) 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 that USPs with periods of less than one day do not form any special group of planets. Rather, this implies that USPs belong to a continuous distribution of super-Earth like planets with periods ranging from the shortest known ones up to ~ 30 days, whose period-radius distribution is delimitated 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 against period, a plateau between periods of 0.6 to 1.4 days has however become notable that 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 and new limits are provided. These limits are also given in terms of the planets' insolation and effective temperatures.