
Anders Johansen
Professor

Resonance in the K2-19 system is at odds with its high reported eccentricities
Author
Summary, in English
K2-19 hosts a planetary system composed of two outer planets, b and c, with size of 7.0 ± 0.2 R⊕ and 4.1 ± 0.2 R⊕, and an inner planet, d, with a radius of 1.11 ± 0.05 R® A recent analysis of Transit-Timing Variations (TTVs) suggested b and c are close to but not in 3:2 mean motion resonance (MMR) because the classical resonant angles circulate. Such an architecture challenges our understanding of planet formation. Indeed, planet migration through the protoplanetary disc should lead to a capture into the MMR. Here, we show that the planets are in fact, locked into the 3:2 resonance despite circulation of the conventional resonant angles and aligned periapses. However, we show that such an orbital configuration cannot be maintained for more than a few hundred million years due to the tidal dissipation experienced by planet d. The tidal dissipation remains efficient because of a secular forcing of the innermost planet eccentricity by planets b and c. While the observations strongly rule out an orbital solution where the three planets are on close to circular orbits, it remains possible that a fourth planet is affecting the TTVs such that the four planet system is consistent with the tidal constraints.
Department/s
- Lund Observatory - Undergoing reorganization
- eSSENCE: The e-Science Collaboration
Publishing year
2020
Language
English
Pages
3101-3111
Publication/Series
Monthly Notices of the Royal Astronomical Society
Volume
496
Issue
3
Document type
Journal article
Publisher
Oxford University Press
Topic
- Astronomy, Astrophysics and Cosmology
Keywords
- Celestial mechanics
- Planets and satellites: Dynamical evolution and stability
- Planets and satellites: Formation
- Planets and satellites: Individual: (K2-19b, K2-19c, K2-19d)
Status
Published
ISBN/ISSN/Other
- ISSN: 0035-8711