TOI-216: Resonant Constraints on Planet Migration
The result's identifiers
Result code in IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F22%3A10456194" target="_blank" >RIV/00216208:11320/22:10456194 - isvavai.cz</a>
Result on the web
<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=4g7Nf-ybum" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=4g7Nf-ybum</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.3847/1538-4357/ac36cd" target="_blank" >10.3847/1538-4357/ac36cd</a>
Alternative languages
Result language
angličtina
Original language name
TOI-216: Resonant Constraints on Planet Migration
Original language description
TOI-216 is a pair of close-in planets with orbits deep in the 2:1 mean motion resonance. The inner Neptune-class planet (TOI-216b) is near 0.12 au (orbital period P (b) similar or equal to 17 days) and has a substantial orbital eccentricity (e (b) similar or equal to 0.16) and large libration amplitude (A ( psi ) similar or equal to 60 degrees) in the resonance. The outer planet (TOI-216c) is a gas giant on a nearly circular orbit. We carry out N-body simulations of planet migration in a protoplanetary gas disk to explain the orbital configuration of TOI-216 planets. We find that TOI-216b's migration must have been halted near its current orbital radius to allow for a convergent migration of the two planets into the resonance. For the inferred damping-to-migration timescale ratio tau ( e )/tau ( a ) similar or equal to 0.02, overstable librations in the resonance lead to a limit cycle with A ( psi ) similar or equal to 80 degrees and e (b) < 0.1. The system could have remained in this configuration for the greater part of the protoplanetary disk lifetime. If the gas disk was removed from inside out, this would have reduced the libration amplitude to A ( psi ) similar or equal to 60 degrees and boosted e (b) via the resonant interaction with TOI-216c. Our results suggest a relatively fast inner-disk removal (similar to 10(5) yr). Another means of explaining the large libration amplitude is stochastic stirring from a (turbulent) gas disk. For that to work, overstable librations would need to be suppressed, tau ( e )/tau ( a ) similar or equal to 0.05, and very strong turbulent stirring (or some other source of large stochastic forcing) would need to overcome the damping effects of gas. Hydrodynamical simulations can be performed to test these models.
Czech name
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Czech description
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Classification
Type
J<sub>imp</sub> - Article in a specialist periodical, which is included in the Web of Science database
CEP classification
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OECD FORD branch
10308 - Astronomy (including astrophysics,space science)
Result continuities
Project
<a href="/en/project/GM21-23067M" target="_blank" >GM21-23067M: Hydrodynamic interactions of planets with protoplanetary disks and the origin of close-in exoplanetary systems</a><br>
Continuities
P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)
Others
Publication year
2022
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Data specific for result type
Name of the periodical
Astrophysical Journal
ISSN
0004-637X
e-ISSN
1538-4357
Volume of the periodical
925
Issue of the periodical within the volume
1
Country of publishing house
US - UNITED STATES
Number of pages
16
Pages from-to
38
UT code for WoS article
000746165800001
EID of the result in the Scopus database
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