TOI-1416: A system with a super-Earth planet with a 1.07d period
Creators: name: Deeg, H. J.
name: Georgieva, I. Y.
name: Nowak, G.
name: Persson, C. M.
name: Cale, B. L.
name: Murgas, F.
name: Pallé, E.
name: Rivera, D. Godoy
name: Dai, F.
name: Ciardi, D. R.
name: Murphy, J. M. Akana
name: Beck, P. G.
name: Burke, C. J.
name: Cabrera, J.
name: Carleo, I.
name: Cochran, W. D.
name: Collins, K. A.
name: Csizmadia, Sz.
name: Mufti, M. El
name: Fridlund, M.
name: Fukui, A.
name: Gandolfi, D.
name: García, R. A.
name: Guenther, E. W.
name: Guerra, P.
name: Grziwa, S.
name: Isaacson, H.
name: Isogai, K.
name: Jenkins, J. M.
name: Kábath, P.
name: Korth, J.
name: Lam, K. W. F.
name: Latham, D. W.
name: Luque, R.
name: Lund, M. B.
name: Livingston, J. H.
name: Mathis, S.
name: Mathur, S.
name: Narita, N.
name: Orell-Miquel, J.
name: Osborne, H. L. M.
name: Parviainen, H.
name: Plavchan, P. P.
name: Redfield, S.
name: Rodriguez, D. R.
name: Schwarz, R. P.
name: Seager, S.
name: Smith, A. M. S.
name: Van Eylen, V.
name: Van Zandt, J.
name: Winn, J. N
name: Ziegler, C.
Publisher: name: arXiv
Year: 2023
Subjects: subject: Earth and Planetary Astrophysics (astro-ph.EP)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: 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.
description: 31 pages, 31 figures, 8 tables, accepted for publication in A&amp;A