Hypervelocity A & B Stars should be slow rotators

Abstract

The most commonly accepted explanation for the origin of hypervelocity stars in the halo of the Milky Way is that they are the result of tidal disruption of binaries by the massive black hole at the center of the Galaxy. We show that, if this scenario is correct, and if the original binary properties are similar to those in the local stellar neighbourhood, then the hypervelocity stars should rotate with velocities measureably lower than those for field stars of similar spectral type. This may prove to be a more direct test of the model than trying to predict the position and velocity distributions.

11 pages, including 4 figures. To appear in Astrophysical Journal Letters

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Cited by in corpus (14)

• MMT Hypervelocity Star Survey III: A Complete Survey of Faint B-type Stars in the Northern Milky Way Halo
• MMT Hypervelocity Star Survey
• Dynamical and evolutionary constraints on the nature and origin of hypervelocity stars
• MMT Hypervelocity Star Survey. II. Five New Unbound Stars
• Tidal breakup of binary stars at the Galactic Center. II. Hydrodynamic simulations
• High velocity stars from close interaction of a globular cluster and a super massive black hole
• On the spatial distribution and the origin of hypervelocity stars
• HVS7: a chemically peculiar hyper-velocity star
• Low Metallicity Indicates that the Hypervelocity Star HE 0437-5439 was Ejected from the LMC
• 'Slow' and Fast Rotators among Hypervelocity Stars
• The spatial and velocity distributions of hypervelocity stars
• The Nature of Hypervelocity Stars and the Time Between Their Formation and Ejection
• The Galactic potential and the asymmetric distribution of hypervelocity stars
• The Origin of HVS17, an Unbound Main Sequence B Star at 50 kpc