Resonance in the K2-19 system is at odds with its high reported eccentricities
(2020) In Monthly Notices of the Royal Astronomical Society 496(3). p.3101-3111- Abstract
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)
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.
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- author
- Petit, Antoine C. LU ; Petigura, Erik A. ; Davies, Melvyn B. LU and Johansen, Anders LU
- organization
- publishing date
- 2020
- type
- Contribution to journal
- publication status
- published
- subject
- keywords
- Celestial mechanics, Planets and satellites: Dynamical evolution and stability, Planets and satellites: Formation, Planets and satellites: Individual: (K2-19b, K2-19c, K2-19d)
- in
- Monthly Notices of the Royal Astronomical Society
- volume
- 496
- issue
- 3
- pages
- 11 pages
- publisher
- Oxford University Press
- external identifiers
-
- scopus:85102148009
- ISSN
- 0035-8711
- DOI
- 10.1093/MNRAS/STAA1736
- language
- English
- LU publication?
- yes
- id
- 342339d9-b9c3-42db-b3eb-fc5ee7cd92fe
- date added to LUP
- 2021-03-22 14:32:21
- date last changed
- 2024-03-05 23:49:25
@article{342339d9-b9c3-42db-b3eb-fc5ee7cd92fe, abstract = {{<p>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.</p>}}, author = {{Petit, Antoine C. and Petigura, Erik A. and Davies, Melvyn B. and Johansen, Anders}}, issn = {{0035-8711}}, keywords = {{Celestial mechanics; Planets and satellites: Dynamical evolution and stability; Planets and satellites: Formation; Planets and satellites: Individual: (K2-19b, K2-19c, K2-19d)}}, language = {{eng}}, number = {{3}}, pages = {{3101--3111}}, publisher = {{Oxford University Press}}, series = {{Monthly Notices of the Royal Astronomical Society}}, title = {{Resonance in the K2-19 system is at odds with its high reported eccentricities}}, url = {{http://dx.doi.org/10.1093/MNRAS/STAA1736}}, doi = {{10.1093/MNRAS/STAA1736}}, volume = {{496}}, year = {{2020}}, }