期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 489, 期 2, 页码 2941-2953出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stz2339
关键词
methods: numerical; celestial mechanics; planets and satellites: detection; planets and satellites: dynamical evolution and stability; planet-star interactions; white dwarfs
资金
- National Science Foundation under the Kavli Institute for Theoretical Physics programme 'Better Stars, Better Planets' [NSF PHY-1748958]
- STFC via an Ernest Rutherford Fellowship [ST/P003850/1]
- Rose Hills Foundation
- Sloan Foundation [FG-2018-10515]
- STFC [ST/P003850/1] Funding Source: UKRI
A gas giant planet which survives the giant branch stages of evolution at a distance of many au and then is subsequently perturbed sufficiently close to a white dwarf will experience orbital shrinkage and circularization due to star-planet tides. The circularization time-scale, when combined with a known white dwarf cooling age, can place coupled constraints on the scattering epoch as well as the active tidal mechanisms. Here, we explore this coupling across the entire plausible parameter phase space by computing orbit shrinkage and potential self-disruption due to chaotic f-mode excitation and heating in planets on orbits with eccentricities near unity, followed by weakly dissipative equilibrium tides. We find that chaotic f-mode evolution activates only for orbital pericentres which are within twice the white dwarf Roche radius, and easily restructures or destroys ice giants but not gas giants. This type of internal thermal destruction provides an additional potential source of white dwarf metal pollution. Subsequent tidal evolution for the surviving planets is dominated by non-chaotic equilibrium and dynamical tides which may be well-constrained by observations of giant planets around white dwarfs at early cooling ages.
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