A binary merger origin for inflated hot Jupiter planets

Bibcode
2011A&A...535A..50M
DOI
10.1051/0004-6361/201116907
Martin, E. L.; Spruit, H. C.; Tata, R.
Referencia bibliográfica

Astronomy and Astrophysics, Volume 535, id.A50

Fecha de publicación:
11
2011
Revista
Astronomy and Astrophysics
Número de autores
3
Número de autores del IAC
1
Número de citas
33
Número de citas referidas
30
Descripción
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.
Tipo
Con árbitro
Métodos

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