The Ultimate Fate of Low-mass Contact Binary Evolution: Planetary System?
Abstract
We follow the idea of Martin et al. (2011) that the formation of hot Jupiters may be related to mergers of cool contact binaries. Contact systems are formed from initially detached binaries with orbital periods around 2-3 d and they end up as mergers. Here we discuss the fate of
binaries with the initial masses ∼ 1.5 M_{⊙} and initial periods shorter than ∼ 2.5 d. These binaries evolve into low-mass contact binaries (LMCB) with periods shorter than 0.3 d and the total mass lower than 1.4 M_{⊙}. After merging, a MS object is formed surrounded by an excretion disk. New planets can be formed in such a disk. The predicted mass distribution of mergers originating from LMCB is in a good agreement with the observed mass distribution of stars hosting possible young planets.- Publication:
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Central European Astrophysical Bulletin
- Pub Date:
- 2013
- Bibcode:
- 2013CEAB...37..381S
- Keywords:
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- planet formation;
- binary evolution;
- contact binaries