Hot Jupiters in binary star systems
Yanqin Wu, Norman W. Murray, J. Michael Ramsahai

TL;DR
This paper proposes that many hot Jupiters form through Kozai mechanism-induced migration in binary star systems, explaining their observed orbital distribution and prevalence.
Contribution
It introduces a model where binary star interactions via Kozai cycles lead to hot Jupiter formation, a novel explanation for their origins.
Findings
Approximately 2.5% of planets migrate inward via Kozai mechanism.
Kozai migration could explain over 10% of hot Jupiters.
Distribution peaks around 3-day orbital periods.
Abstract
Radial velocity surveys find Jupiter mass planets with semi-major axes a less than 0.1 AU around ~1% of solar-type stars; counting planets with as large as 5 AU, the fraction of stars having planets reaches ~ 10% {Marcy,Butler}. An examination of the distribution of semi-major axes shows that there is a clear excess of planets with orbital periods around 3 or 4 days, corresponding to a~0.03$ AU, with a sharp cutoff at shorter periods (see Figure 1). It is believed that Jupiter mass planets form at large distances from their parent stars; some fraction then migrate in to produce the short period objects. We argue that a significant fraction of the `hot Jupiters' (a<0.1 AU) may arise in binary star systems in which the orbit of the binary is highly inclined to the orbit of the planet. Mutual torques between the two orbits drive down the minimum separation or periapse r_p between the…
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