SIMBAD references

2019ApJ...873..116H - Astrophys. J., 873, 116-116 (2019/March-2)

Origin of a massive hyper-runaway subgiant star LAMOST-HVS1: implication from Gaia and follow-up spectroscopy.

HATTORI K., VALLURI M., CASTRO N., ROEDERER I.U., MAHLER G. and KHULLAR G.

Abstract (from CDS):

We report that LAMOST-HVS1 is a massive hyper-runaway subgiant star with a mass of 8.3 M and super-solar metallicity, which was ejected from the inner stellar disk of the Milky Way ∼33 Myr ago with the intrinsic ejection velocity of 568–17+19kms–1 (corrected for the streaming motion of the disk), based on the proper motion data from Gaia Data Release 2 (DR2) and high-resolution spectroscopy. The extremely large ejection velocity indicates that this star was not ejected by the supernova explosion of a binary companion. Rather, it was probably ejected by a three- or four-body dynamical interaction with more massive objects in a high-density environment. Such a high-density environment may be attained at the core region of a young massive cluster (YMC) with mass of >=104 M. The ejection agent that took part in the ejection of LAMOST-HVS1 may be an intermediate mass black hole (>=100 M), a very massive star (>=100 M), or multiple ordinary massive stars (>=30 M). Based on the flight time and the ejection location of LAMOST-HVS1, we argue that its ejection agent or its natal star cluster is currently located near the Norma spiral arm. The natal star cluster of LAMOST-HVS1 may be an undiscovered YMC near the Norma spiral arm.

Abstract Copyright: © 2019. The American Astronomical Society. All rights reserved.

Journal keyword(s): Galaxy: disk - Galaxy: kinematics and dynamics - open clusters and associations: general - stars: abundances - stars: early-type - stars: individual: LAMOST-HVS1

Simbad objects: 17

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2019.09.23-05:58:15

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