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

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F23%3A00576950" target="_blank" >RIV/67985815:_____/23:00576950 - isvavai.cz</a>

Výsledek na webu

<a href="https://hdl.handle.net/11104/0347225" target="_blank" >https://hdl.handle.net/11104/0347225</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/202346370" target="_blank" >10.1051/0004-6361/202346370</a>

Jazyk výsledku

angličtina

Název v původním jazyce

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

Popis výsledku v původním jazyce

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 TOI1416 b, which has a mass of 3.48 +/- 0.47 M-circle plus and a radius of 1.62 +/- 0.08 R-circle plus, implying a slightly sub-Earth density of 4.50(-0.83)(+0.99) 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 (T-eq approximate to 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 approximate 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-circle plus and a mass of 0.028 M-jup (corresponding to 8.9 M-circle plus) as the desert's lower limits. We also provide corresponding limits to the Neptune Desert against the planets' insolation and effective temperatures.

Název v anglickém jazyce

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

Popis výsledku anglicky

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 TOI1416 b, which has a mass of 3.48 +/- 0.47 M-circle plus and a radius of 1.62 +/- 0.08 R-circle plus, implying a slightly sub-Earth density of 4.50(-0.83)(+0.99) 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 (T-eq approximate to 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 approximate 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-circle plus and a mass of 0.028 M-jup (corresponding to 8.9 M-circle plus) as the desert's lower limits. We also provide corresponding limits to the Neptune Desert against the planets' insolation and effective temperatures.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

—

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2023

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název periodika

Astronomy & Astrophysics

ISSN

0004-6361

e-ISSN

1432-0746

Svazek periodika

677

Číslo periodika v rámci svazku

September

Stát vydavatele periodika

FR - Francouzská republika

Počet stran výsledku

29

Strana od-do

A12

Kód UT WoS článku

001063425400004

EID výsledku v databázi Scopus

2-s2.0-85170822852