Planetesimals Pile Up in Binary Systems

Astronomy and Astrophysics – Astronomy

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Scientific paper

We investigate the radial migration and accretion condition of 1-100 km-sized planetesimals in binary star systems. Comparing the results to those in single star systems, we focus on the effects of the binary's orbital semi-major axis(aB), eccentricity(e_B), and inclination(iB). We find that if iB> 10o, highly significant binary effects(being very different from that in single star systems) occur: (1) planetesimal begin to pile up in inner region, at roughly 0.02aB-0.03aB, leading to typical local surface density enhancement of 1 order of magnitude on a time scale of 105 yrs, (2) furthermore, if iB> 80o, planetesimals directly ``jump inward" and pile up within 1 AU, resulting in a surface density enhancement of as much as 2 orders of magnitude on Kozai timescale. We then investigate the conditions for planetesimal mutual accretion at these planetesimal piling region, and it is found to be nearly unperturbed by the companion star, namely almost as accretion-friendly as in single star systems. Because of planetesimal piling up, planetary embryos (or gas giant cores) can be formed efficiently with much larger isolation mass in inner region. As iB > 10o is very common for binary systems, we predict that more massive planets(or planets with massive cores) with short orbital periods would be discovered in binary systems than in single star systems. This mass-period correlation will be tested by the ongoing MARVELS.
We would like to thank the W.M. Keck Foundation, NSF, SDSS-III consortium, NASA and UF for support.

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