Transit timing variation signature of planet migration: The case of K2-24

Jean Teyssandier; Anne Sophie Libert

doi:10.1051/0004-6361/202039038

Transit timing variation signature of planet migration: The case of K2-24

Jean Teyssandier, Anne Sophie Libert

University of Namur

Research output: Contribution to journal › Article › peer-review

Abstract

The convergent migration of two planets in a gaseous disc can lead to mean motion resonance (MMR) capture. In addition, pairs of planets in or near MMRs are known to produce strong transit timing variations (TTVs). In this paper, we study the impact of disc-induced migrations on the TTV signal of pairs of planets that enter a resonant configuration. We show that disc-induced migration creates a correlation between the amplitude and the period of the TTVs. We study the case of K2-24, a system of two planets whose period ratio indicates that they are in or near the 2:1 MMR, with non-zero eccentricities and large-amplitude TTVs. We show that a simple disc-induced migration cannot reproduce the observed TTVs. Moreover, we propose a formation scenario in which the capture in resonance during migration in a disc with strong eccentricity damping is followed by eccentricity excitation during the dispersal of the disc. This is assisted by a third planet whose presence has been suggested by radial velocity observations. This scenario accounts for the eccentricities of the two planets and their period ratio, and it accurately reproduces the amplitude and period of the TTVs. It allows for a unified view of the formation and evolution history of K2-24, from disc-induced migration to its currently observed properties.

Original language	English
Article number	A11
Journal	Astronomy and Astrophysics
Volume	643
DOIs	https://doi.org/10.1051/0004-6361/202039038
Publication status	Published - 1 Nov 2020

Funding

Acknowledgements. The work of J.T. is supported by a Fonds de la Recherche Sci-entifique – FNRS Postdoctoral Research Fellowship. Computational resources have been provided by the PTCI (Consortium des Équipements de Calcul Intensif CECI), funded by the FNRS-FRFC, the Walloon Region, and the University of Namur (Conventions No. 2.5020.11, GEQ U.G006.15, 1610468 and RW/GEQ2016). The research done in this project made use of the SciPy stack (Jones et al. 2001), including NumPy (Oliphant 2006) and Matplotlib (Hunter 2007), as well as Astropy (http://www.astropy.org), a community-developed core Python package for Astronomy (Astropy Collaboration 2013, 2018). Simulations in this paper made use of the REBOUND code which is freely available at http://github.com/hannorein/rebound.

Keywords

Celestial mechanics
Planet-disk interactions
Planets and satellites: detection
Planets and satellites: dynamical evolution and stability
Planets and satellites: formation
Protoplanetary disks

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10.1051/0004-6361/202039038

Cite this

@article{c3752b018978428f9e9a0747490ed518,

title = "Transit timing variation signature of planet migration: The case of K2-24",

abstract = "The convergent migration of two planets in a gaseous disc can lead to mean motion resonance (MMR) capture. In addition, pairs of planets in or near MMRs are known to produce strong transit timing variations (TTVs). In this paper, we study the impact of disc-induced migrations on the TTV signal of pairs of planets that enter a resonant configuration. We show that disc-induced migration creates a correlation between the amplitude and the period of the TTVs. We study the case of K2-24, a system of two planets whose period ratio indicates that they are in or near the 2:1 MMR, with non-zero eccentricities and large-amplitude TTVs. We show that a simple disc-induced migration cannot reproduce the observed TTVs. Moreover, we propose a formation scenario in which the capture in resonance during migration in a disc with strong eccentricity damping is followed by eccentricity excitation during the dispersal of the disc. This is assisted by a third planet whose presence has been suggested by radial velocity observations. This scenario accounts for the eccentricities of the two planets and their period ratio, and it accurately reproduces the amplitude and period of the TTVs. It allows for a unified view of the formation and evolution history of K2-24, from disc-induced migration to its currently observed properties. ",

keywords = "Celestial mechanics, Planet-disk interactions, Planets and satellites: detection, Planets and satellites: dynamical evolution and stability, Planets and satellites: formation, Protoplanetary disks",

author = "Jean Teyssandier and Libert, {Anne Sophie}",

note = "Funding Information: Acknowledgements. The work of J.T. is supported by a Fonds de la Recherche Sci-entifique – FNRS Postdoctoral Research Fellowship. Computational resources have been provided by the PTCI (Consortium des {\'E}quipements de Calcul Intensif CECI), funded by the FNRS-FRFC, the Walloon Region, and the University of Namur (Conventions No. 2.5020.11, GEQ U.G006.15, 1610468 and RW/GEQ2016). The research done in this project made use of the SciPy stack (Jones et al. 2001), including NumPy (Oliphant 2006) and Matplotlib (Hunter 2007), as well as Astropy (http://www.astropy.org), a community-developed core Python package for Astronomy (Astropy Collaboration 2013, 2018). Simulations in this paper made use of the REBOUND code which is freely available at http://github.com/hannorein/rebound. Publisher Copyright: {\textcopyright} 2020 ESO. Copyright: Copyright 2020 Elsevier B.V., All rights reserved.",

year = "2020",

month = nov,

day = "1",

doi = "10.1051/0004-6361/202039038",

language = "English",

volume = "643",

journal = "Astronomy and Astrophysics",

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N2 - The convergent migration of two planets in a gaseous disc can lead to mean motion resonance (MMR) capture. In addition, pairs of planets in or near MMRs are known to produce strong transit timing variations (TTVs). In this paper, we study the impact of disc-induced migrations on the TTV signal of pairs of planets that enter a resonant configuration. We show that disc-induced migration creates a correlation between the amplitude and the period of the TTVs. We study the case of K2-24, a system of two planets whose period ratio indicates that they are in or near the 2:1 MMR, with non-zero eccentricities and large-amplitude TTVs. We show that a simple disc-induced migration cannot reproduce the observed TTVs. Moreover, we propose a formation scenario in which the capture in resonance during migration in a disc with strong eccentricity damping is followed by eccentricity excitation during the dispersal of the disc. This is assisted by a third planet whose presence has been suggested by radial velocity observations. This scenario accounts for the eccentricities of the two planets and their period ratio, and it accurately reproduces the amplitude and period of the TTVs. It allows for a unified view of the formation and evolution history of K2-24, from disc-induced migration to its currently observed properties.

AB - The convergent migration of two planets in a gaseous disc can lead to mean motion resonance (MMR) capture. In addition, pairs of planets in or near MMRs are known to produce strong transit timing variations (TTVs). In this paper, we study the impact of disc-induced migrations on the TTV signal of pairs of planets that enter a resonant configuration. We show that disc-induced migration creates a correlation between the amplitude and the period of the TTVs. We study the case of K2-24, a system of two planets whose period ratio indicates that they are in or near the 2:1 MMR, with non-zero eccentricities and large-amplitude TTVs. We show that a simple disc-induced migration cannot reproduce the observed TTVs. Moreover, we propose a formation scenario in which the capture in resonance during migration in a disc with strong eccentricity damping is followed by eccentricity excitation during the dispersal of the disc. This is assisted by a third planet whose presence has been suggested by radial velocity observations. This scenario accounts for the eccentricities of the two planets and their period ratio, and it accurately reproduces the amplitude and period of the TTVs. It allows for a unified view of the formation and evolution history of K2-24, from disc-induced migration to its currently observed properties.

KW - Celestial mechanics

KW - Planet-disk interactions

KW - Planets and satellites: detection

KW - Planets and satellites: dynamical evolution and stability

KW - Planets and satellites: formation

KW - Protoplanetary disks

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DO - 10.1051/0004-6361/202039038

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SN - 0004-6361

VL - 643

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A11

ER -

Transit timing variation signature of planet migration: The case of K2-24

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Transit timing variation signature of planet migration: The case of K2-24

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