학술논문
TOI-1416: A system with a super-Earth planet with a 1.07d period
Document Type
Working Paper
Author
Deeg, H. J.; Georgieva, I. Y.; Nowak, G.; Persson, C. M.; Cale, B. L.; Murgas, F.; Pallé, E.; Rivera, D. Godoy; Dai, F.; Ciardi, D. R.; Murphy, J. M. Akana; Beck, P. G.; Burke, C. J.; Cabrera, J.; Carleo, I.; Cochran, W. D.; Collins, K. A.; Csizmadia, Sz.; Mufti, M. El; 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.; Van Eylen, V.; Van Zandt, J.; Winn, J. N; Ziegler, C.
Source
A&A 677, A12 (2023)
Subject
Language
Abstract
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.
Comment: 31 pages, 31 figures, 8 tables, accepted for publication in A&A
Comment: 31 pages, 31 figures, 8 tables, accepted for publication in A&A