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2016ApJ...829..114B - Astrophys. J., 829, 114-114 (2016/October-1)

In situ formation and dynamical evolution of hot Jupiter systems.


Abstract (from CDS):

Hot Jupiters, giant extrasolar planets with orbital periods shorter than ∼10 days, have long been thought to form at large radial distances, only to subsequently experience long-range inward migration. Here, we offer the contrasting view that a substantial fraction of the hot Jupiter population formed in situ via the core-accretion process. We show that under conditions appropriate to the inner regions of protoplanetary disks, rapid gas accretion can be initiated by super-Earth-type planets, comprising 10-20 Earth masses of refractory material. An in situ formation scenario leads to testable consequences, including the expectation that hot Jupiters should frequently be accompanied by additional low-mass planets with periods shorter than ∼100 days. Our calculations further demonstrate that dynamical interactions during the early stages of planetary systems' lifetimes should increase the inclinations of such companions, rendering transits rare. High-precision radial velocity monitoring provides the best prospect for their detection.

Abstract Copyright: © 2016. The American Astronomical Society. All rights reserved.

Journal keyword(s): planets and satellites: dynamical evolution and stability - planets and satellites: formation - planets and satellites: formation

Simbad objects: 9

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