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Title:
Substellar companions and isolated planetary-mass objects from protostellar disc fragmentation
Authors:
Rice, W. K. M.; Armitage, P. J.; Bonnell, I. A.; Bate, M. R.; Jeffers, S. V.; Vine, S. G.
Affiliation:
AA(School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews KY16 9SS), AB(JILA, Campus Box 440, University of Colorado, Boulder, CO 80309-0440, USA; Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, CO 80309-0391, USA), AC(School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews KY16 9SS), AD(School of Physics, University of Exeter, Stocker Road, Exeter EX4 4QL), AE(School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews KY16 9SS), AF(School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews KY16 9SS)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 346, Issue 3, pp. L36-L40. (MNRAS Homepage)
Publication Date:
12/2003
Origin:
MNRAS
Astronomy Keywords:
accretion, accretion discs, planets and satellites: formation, stars: low-mass, brown dwarfs, planetary systems: protoplanetary discs, stars: pre-main sequence
DOI:
10.1111/j.1365-2966.2003.07317.x
Bibliographic Code:
2003MNRAS.346L..36R

Abstract

Self-gravitating protostellar discs are unstable to fragmentation if the gas can cool on a time-scale that is short compared with the orbital period. We use a combination of hydrodynamic simulations and N-body orbit integrations to study the long-term evolution of a fragmenting disc with an initial mass ratio to the star of Mdisc/M*= 0.1. For a disc that is initially unstable across a range of radii, a combination of collapse and subsequent accretion yields substellar objects with a spectrum of masses extending (for a Solar-mass star) up to ~0.01 Msolar. Subsequent gravitational evolution ejects most of the lower mass objects within a few million years, leaving a small number of very massive planets or brown dwarfs in eccentric orbits at moderately small radii. Based on these results, systems such as HD 168443 - in which the companions are close to or beyond the deuterium burning limit - appear to be the best candidates to have formed via gravitational instability. If massive substellar companions originate from disc fragmentation, while lower-mass planetary companions originate from core accretion, the metallicity distribution of stars which host massive substellar companions at radii of ~1 au should differ from that of stars with lower mass planetary companions.

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