TOI-1416: A system with a super-Earth planet with a 1.07 d period
Artikel i vetenskaplig tidskrift, 2023
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 TOI-1416 b, which has a mass of 3.48 ± 0.47 M• and a radius of 1.62 ± 0.08 R•, implying a slightly sub-Earth density of 4.500.83+0.99 g cm3. 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 ≈ 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 ≈ 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• and a mass of 0.028 Mjup (corresponding to 8.9 M•) as the desert s lower limits. We also provide corresponding limits to the Neptune Desert against the planets insolation and effective temperatures.
Planets and satellites: composition
Planets and satellites: detection
Planets and satellites: individual: TOI-1416 b
Planetary systems
Techniques: radial velocities
Planets and satellites: terrestrial planets
Författare
H. Deeg
Instituto de Astrofísica de Canarias
Universidad de la Laguna
Iskra Georgieva
Chalmers, Rymd-, geo- och miljövetenskap, Astronomi och plasmafysik
G. Nowak
Instituto de Astrofísica de Canarias
Uniwersytet Mikolaja Kopernika
Universidad de la Laguna
Carina Persson
Chalmers, Rymd-, geo- och miljövetenskap, Astronomi och plasmafysik
B. Cale
National Aeronautics and Space Administration (NASA)
F. Murgas
Instituto de Astrofísica de Canarias
Universidad de la Laguna
Enric Palle
Universidad de la Laguna
Instituto de Astrofísica de Canarias
D. Godoy-Rivera
Instituto de Astrofísica de Canarias
Universidad de la Laguna
F. Dai
California Institute of Technology (Caltech)
D. R. Ciardi
National Aeronautics and Space Administration (NASA)
J. M.Akana Murphy
University of California
P. G. Beck
Instituto de Astrofísica de Canarias
Universidad de la Laguna
Karl-Franzens-Universität Graz
Christopher J. Burke
Massachusetts Institute of Technology (MIT)
J. Cabrera
Deutsches Zentrums für Luft- und Raumfahrt (DLR)
Ilaria Carleo
Wesleyan University
Universidad de la Laguna
Instituto de Astrofísica de Canarias
William D. Cochran
The University of Texas at Austin
Karen A. Collins
Harvard-Smithsonian Center for Astrophysics
Szilard Csizmadia
Deutsches Zentrums für Luft- und Raumfahrt (DLR)
M. El Mufti
George Mason University
Malcolm Fridlund
Universiteit Leiden
Chalmers, Rymd-, geo- och miljövetenskap, Astronomi och plasmafysik
A. Fukui
University of Tokyo
Instituto de Astrofísica de Canarias
D. Gandolfi
Universita degli Studi di Torino
R. A. García
Institut de Recherche sur les Lois Fondamentales de l'Univers
E. W. Guenther
Thüringer Landessternwarte Tautenburg
P. Guerra
Observatori Astronòmic Albanya
S. Grziwa
Universität zu Köln
H. Isaacson
University of California
University of Southern Queensland
K. Isogai
University of Tokyo
Kyoto University
Jon M. Jenkins
NASA Ames Research Center
Petr Kabath
Czech Academy of Sciences
Judith Korth
Chalmers, Rymd-, geo- och miljövetenskap, Astronomi och plasmafysik
K. W.F. Lam
Deutsches Zentrums für Luft- und Raumfahrt (DLR)
D. W. Latham
Harvard-Smithsonian Center for Astrophysics
R. Luque
Universidad de la Laguna
University of Chicago
Instituto de Astrofísica de Canarias
M. B. Lund
National Aeronautics and Space Administration (NASA)
J.H. Livingston
National Institutes of Natural Sciences
The Graduate University for Advanced Studies (SOKENDAI)
National Astronomical Observatory of Japan
S. Mathis
Institut de Recherche sur les Lois Fondamentales de l'Univers
S. Mathur
Instituto de Astrofísica de Canarias
Universidad de la Laguna
Norio Narita
National Institutes of Natural Sciences
Instituto de Astrofísica de Canarias
University of Tokyo
J. Orell-Miquel
Instituto de Astrofísica de Canarias
Universidad de la Laguna
H. L.M. Osborne
University College London (UCL)
H. Parviainen
Instituto de Astrofísica de Canarias
Universidad de la Laguna
P. Plavchan
George Mason University
S. Redfield
Wesleyan University
D. R. Rodriguez
Space Telescope Science Institute (STScI)
R. Schwarz
Harvard-Smithsonian Center for Astrophysics
S. Seager
Massachusetts Institute of Technology (MIT)
A. M.S. Smith
Deutsches Zentrums für Luft- und Raumfahrt (DLR)
Vincent Van Eylen
University College London (UCL)
J. Van Zandt
University of California
J. N. Winn
Princeton University
C. Ziegler
Stephen F. Austin State University
Astronomy and Astrophysics
0004-6361 (ISSN) 1432-0746 (eISSN)
Vol. 677 A12Ämneskategorier
Astronomi, astrofysik och kosmologi
DOI
10.1051/0004-6361/202346370