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2012MNRAS.419.2448P - Mon. Not. R. Astron. Soc., 419, 2448-2458 (2012/January-3)
The effects of dynamical interactions on planets in young substructured star clusters.
PARKER R.J. and QUANZ S.P.
Abstract (from CDS):
Of the planets that become free-floating, those that remain observationally associated with the cluster (i.e. within two half-mass radii of the cluster centre) have a similar velocity distribution to the entire star cluster, irrespective of whether they were on a 5 or 30 au orbit, with median velocities typically ∼ 1 km/s. Conversely, those planets that are no longer associated with the cluster have similar velocities to the non-associated stars if they were originally at 5 au ( ∼ 9 km/s), whereas the planets originally at 30 au have much lower velocities (3.8 km/s) than the non-associated stars (10.8 km/s). These findings highlight potential pitfalls of concluding that (a) planets with similar velocities to the cluster stars represent the very low mass end of the initial mass function and (b) planets on the periphery of a cluster with very different observed velocities form through different mechanisms. The spectral variability and magnetic field characteristics of the Of?p star HD 148937
Abstract Copyright: 2011 The Authors Monthly Notices of the Royal Astronomical Society2011 RAS
Journal keyword(s): methods: numerical - planet-star interactions - stars: formation - stars: kinematics and dynamics - planetary systems - open clusters and associations: general
Simbad objects: 12
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