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Three Terrestrial Planets Transiting Mid-to-Late M Dwarfs and Constraints on the Occurrence of Such Worlds.

Record Type:	Electronic resources : Monograph/item
Title/Author:	Three Terrestrial Planets Transiting Mid-to-Late M Dwarfs and Constraints on the Occurrence of Such Worlds./
Author:	Ment, Kristo.
Description:	1 online resource (202 pages)
Notes:	Source: Dissertations Abstracts International, Volume: 84-12, Section: B.
Contained By:	Dissertations Abstracts International84-12B.
Subject:	Astronomy. -
Online resource:	http://pqdd.sinica.edu.tw/twdaoapp/servlet/advanced?query=30492640click for full text (PQDT)
ISBN:	9798379614935

Three Terrestrial Planets Transiting Mid-to-Late M Dwarfs and Constraints on the Occurrence of Such Worlds.
Ment, Kristo.

Three Terrestrial Planets Transiting Mid-to-Late M Dwarfs and Constraints on the Occurrence of Such Worlds. - 1 online resource (202 pages)

Source: Dissertations Abstracts International, Volume: 84-12, Section: B.

Thesis (Ph.D.)--Harvard University, 2023.

Includes bibliographical references

While the planet population around Solar-type stars has been relatively well studied and characterized, the same cannot be said for the least massive stars with masses below 0.3 M⊙. Planet formation and evolution processes are dependent on stellar mass as well as irradiation environment. I aim to constrain the occurrence rate of planets within a volume-complete sample of mid-to-late M dwarfs with masses between 0.1- 0.3 M⊙ within 15 pc of the Sun. To this end, I first present the discoveries of three terrestrial planets within that sample, found via the transit method. I then proceed to estimate the incidence rate of such worlds through a thorough investigation of TESS photometric data.I present the discovery of LHS 1140 c, a terrestrial planet with a mass of 1.81±0.39 M⊕ and a radius of 1.28 ± 0.02 R⊕ on a 3.78-day orbit around a nearby M dwarf. This planet was identified from a single transit observation to which the trained neural network assigned a low probability of being caused by atmospheric variations or telescope systematics. I then present the discovery of TOI 540 b, a sub-Earth-sized planet with a radius of 0.90 ± 0.05 R⊕ on a 1.24-day orbit around a magnetically active M dwarf. The star has a high X-ray luminosity and is one of the few known M dwarf planetary systems where the stellar rotation period (17.4 hours) is shorter than the orbital period of the planet. Finally, I announce the discovery of LHS 475 b, another terrestrial planet with a radius of 0.96 ± 0.02 R⊕ on a 2.03-day orbit around an M dwarf 12.5 pc from the Sun.I produce independent estimates of planet detection sensitivity for every mid-tolate M dwarf within the 15 pc sample observed by TESS as a function of orbital period, planet radius, and insolation. The median mass of this sample is 0.17 M⊙. I calculate a cumulative occurrence rate of 0.61+0.24−0.19 planets with orbital periods less than 7 days and radii above 0.5 R⊕ per M dwarf. This corresponds to an incidence rate of 0.49+0.19−0.15 planets per star with insolations above 4 S⊕. I find that for insolations above 4 S⊕, rocky planets heavily outnumber non-rocky planets around low-mass M dwarfs at a ratio of 13 to 1, in contrast to the planet population around early M dwarfs (median mass 0.50 M⊙) where rocky and non-rocky planets are equally abundant. I place an upper limit of 0.07 planets with radii above 1.5 R⊕ per mid-to-late M dwarf, within the orbital period range of 0.5-7 days. The cumulative occurrence rate of planets with insolations above 4 S⊕ is lower around mid-to-late M dwarfs (0.17 M⊙) than it is around early M dwarfs (0.50 M⊙), in contrast with previous studies that have found an inverse correlation between planet incidence and stellar mass amongst early-M and FGK dwarfs.

Electronic reproduction.
Ann Arbor, Mich. :
ProQuest,
2023

Mode of access: World Wide Web

ISBN: 9798379614935Subjects--Topical Terms:

517668
Astronomy.
Subjects--Index Terms:

ExoplanetsIndex Terms--Genre/Form:

542853
Electronic books.

Three Terrestrial Planets Transiting Mid-to-Late M Dwarfs and Constraints on the Occurrence of Such Worlds.
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504 $a Includes bibliographical references
520 $a While the planet population around Solar-type stars has been relatively well studied and characterized, the same cannot be said for the least massive stars with masses below 0.3 M⊙. Planet formation and evolution processes are dependent on stellar mass as well as irradiation environment. I aim to constrain the occurrence rate of planets within a volume-complete sample of mid-to-late M dwarfs with masses between 0.1- 0.3 M⊙ within 15 pc of the Sun. To this end, I first present the discoveries of three terrestrial planets within that sample, found via the transit method. I then proceed to estimate the incidence rate of such worlds through a thorough investigation of TESS photometric data.I present the discovery of LHS 1140 c, a terrestrial planet with a mass of 1.81±0.39 M⊕ and a radius of 1.28 ± 0.02 R⊕ on a 3.78-day orbit around a nearby M dwarf. This planet was identified from a single transit observation to which the trained neural network assigned a low probability of being caused by atmospheric variations or telescope systematics. I then present the discovery of TOI 540 b, a sub-Earth-sized planet with a radius of 0.90 ± 0.05 R⊕ on a 1.24-day orbit around a magnetically active M dwarf. The star has a high X-ray luminosity and is one of the few known M dwarf planetary systems where the stellar rotation period (17.4 hours) is shorter than the orbital period of the planet. Finally, I announce the discovery of LHS 475 b, another terrestrial planet with a radius of 0.96 ± 0.02 R⊕ on a 2.03-day orbit around an M dwarf 12.5 pc from the Sun.I produce independent estimates of planet detection sensitivity for every mid-tolate M dwarf within the 15 pc sample observed by TESS as a function of orbital period, planet radius, and insolation. The median mass of this sample is 0.17 M⊙. I calculate a cumulative occurrence rate of 0.61+0.24−0.19 planets with orbital periods less than 7 days and radii above 0.5 R⊕ per M dwarf. This corresponds to an incidence rate of 0.49+0.19−0.15 planets per star with insolations above 4 S⊕. I find that for insolations above 4 S⊕, rocky planets heavily outnumber non-rocky planets around low-mass M dwarfs at a ratio of 13 to 1, in contrast to the planet population around early M dwarfs (median mass 0.50 M⊙) where rocky and non-rocky planets are equally abundant. I place an upper limit of 0.07 planets with radii above 1.5 R⊕ per mid-to-late M dwarf, within the orbital period range of 0.5-7 days. The cumulative occurrence rate of planets with insolations above 4 S⊕ is lower around mid-to-late M dwarfs (0.17 M⊙) than it is around early M dwarfs (0.50 M⊙), in contrast with previous studies that have found an inverse correlation between planet incidence and stellar mass amongst early-M and FGK dwarfs.
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