Multiple-planet system resonances Virtual Observatory Resource

Authors
  1. Hamer J.H.
  2. Schlaufman K.C.
  3. Published by
    CDS
Abstract

Before the launch of the Kepler Space Telescope, models of low-mass planet formation predicted that convergent type I migration would often produce systems of low-mass planets in low-order mean-motion resonances. Instead, Kepler discovered that systems of small planets frequently have period ratios larger than those associated with mean-motion resonances and rarely have period ratios smaller than those associated with mean-motion resonances. Both short-timescale processes related to the formation or early evolution of planetary systems and long-timescale secular processes have been proposed as explanations for these observations. Using a thin disk stellar population's Galactic velocity dispersion as a relative age proxy, we find that Kepler-discovered multiple-planet systems with at least one planet pair near a period ratio suggestive of a second-order mean-motion resonance have a colder Galactic velocity dispersion and are therefore younger than both single-transiting and multiple-planet systems that lack planet pairs consistent with mean-motion resonances. We argue that a nontidal secular process with a characteristic timescale no less than a few hundred Myr is responsible for moving systems of low-mass planets away from second-order mean-motion resonances. Among systems with at least one planet pair near a period ratio suggestive of a first-order mean-motion resonance, only the population of systems likely affected by tidal dissipation inside their innermost planets has a small Galactic velocity dispersion and is therefore young. We predict that period ratios suggestive of mean-motion resonances are more common in young systems with 10Myr<~{tau}<~100Myr and become less common as planetary systems age.

Keywords
  1. exoplanets
  2. visible-astronomy
Bibliographic source Bibcode
2024AJ....167...55H
See also HTML
https://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/167/55
IVOA Identifier IVOID
ivo://CDS.VizieR/J/AJ/167/55

Access

Web browser access HTML
http://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/AJ/167/55
https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/AJ/167/55
http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/AJ/167/55
IVOA Table Access TAP
http://tapvizier.cds.unistra.fr/TAPVizieR/tap
Run SQL-like queries with TAP-enabled clients (e.g., TOPCAT).
IVOA Cone Search SCS
For use with a cone search client (e.g., TOPCAT).
https://vizier.cds.unistra.fr/viz-bin/conesearch/J/AJ/167/55/table1?
https://vizier.iucaa.in/viz-bin/conesearch/J/AJ/167/55/table1?
http://vizieridia.saao.ac.za/viz-bin/conesearch/J/AJ/167/55/table1?
IVOA Cone Search SCS
For use with a cone search client (e.g., TOPCAT).
https://vizier.cds.unistra.fr/viz-bin/conesearch/J/AJ/167/55/table2?
https://vizier.iucaa.in/viz-bin/conesearch/J/AJ/167/55/table2?
http://vizieridia.saao.ac.za/viz-bin/conesearch/J/AJ/167/55/table2?

History

2025-03-04T16:44:30Z
Resource record created
2025-03-04T16:00:11Z
Updated
2025-03-04T16:44:30Z
Created

Contact

Name
CDS support team
Postal Address
CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France
E-Mail
cds-question@unistra.fr