A binary merger origin for inflated hot Jupiter planets

Details A binary merger origin for inflated hot Jupiter planets A binary merger origin for inflated hot Jupiter planets

2011-02-16

arxiv.org/abs/1102.3336v3

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

Accepted for publication in A&A

Scientific paper

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.

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