A binary merger origin for inflated hot Jupiter planets
Abstract
We hypothesize that hot Jupiters with inflated sizes represent a separate planet formation channel,the merging of two low-mass stars. We show that the abundance and properties of W UMa stars and low mass detached binaries are consistent with their being possible progenitors. The degree of inflation of the transiting hot Jupiters correlates with their expected spiral-in life time by tidal dissipation, and this could indicate youth if the stellar dissipation parameter Q'* is sufficiently low. Several Jupiter-mass planets can form in the massive compact disk formed in a merger event. Gravitational scattering between them can explain the high incidence of excentric, inclined, and retrograde orbits. If the population of inflated planets is indeed formed by a merger process, their frequency should be much higher around blue stragglers than around T Tauri stars.
Cite
@article{arxiv.1102.3336,
title = {A binary merger origin for inflated hot Jupiter planets},
author = {E. L. Martin and H. C. Spruit and R. Tata},
journal= {arXiv preprint arXiv:1102.3336},
year = {2015}
}
Comments
Accepted for publication in A&A