TOI-1416 radial velocities

DOI

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 455ppm and a period of 1.07 days. Radial velocities (RVs) confirm the presence of the transiting planet TOI-1416 b, which has a mass of 3.48+/-0.47M_{Earth} and a radius of 1.62+/-0.08R{Earth}, implying a slightly sub-Earth density of 4.50^+0.90^-0.83_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 (Teq=~1570K) 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 =~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 1.6R_{Earth} and a mass of 0.028M_jup (corresponding to 8.9M_{Earth}_) as the desert's lower limits. We also provide corresponding limits to the Neptune Desert against the planets' insolation and effective temperatures.

Identifier
DOI http://doi.org/10.26093/cds/vizier.36770012
Source https://dc.g-vo.org/rr/q/lp/custom/CDS.VizieR/J/A+A/677/A12
Related Identifier https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/677/A12
Related Identifier http://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/677/A12
Metadata Access http://dc.g-vo.org/rr/q/pmh/pubreg.xml?verb=GetRecord&metadataPrefix=oai_b2find&identifier=ivo://CDS.VizieR/J/A+A/677/A12
Provenance
Creator Deeg H.J.; Georgieva I.Y.; Nowak G.; Persson C.M.; Cale B.L.; Murgas F.,Palle E.; Godoy-Rivera D.; 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.; El Mufti M.; Fridlund M.; Fukui A.; Gandolfi D.; Garcia R.A.,Guenther E.W.; Guerra P.; Grziwa S.; Isaacson H.; Isogai K.; Jenkins J.M.,Kabath 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.
Publisher CDS
Publication Year 2023
Rights https://cds.unistra.fr/vizier-org/licences_vizier.html
OpenAccess true
Contact CDS support team <cds-question(at)unistra.fr>
Representation
Resource Type Dataset; AstroObjects
Discipline Astrophysics and Astronomy; Exoplanet Astronomy; Natural Sciences; Observational Astronomy; Physics; Stellar Astronomy