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2006MNRAS.366L..31K - Mon. Not. R. Astron. Soc., 366, L31-L34 (2006/February-2)
The faintest accretors.
KING A.R. and WIJNANDS R.
Abstract (from CDS):
Two other explanations appear to be quite natural. One invokes accretion by neutron stars or stellar-mass black holes from companions that were already brown dwarfs or planets when the systems formed, i.e. which did not descend from low-mass stars. The other possibility is that these systems are the endpoints of primordial (zero-metallicity) binaries in which the primary was extremely massive, and collapsed to a black hole of mass ≳1000M☉. The (primordial) companion must by now have reached an extremely low mass (≲0.01M☉) and be transferring mass at a very low rate to the black hole. This picture avoids the main difficulty encountered by models invoking intermediate-mass black hole formation at non-primordial metallicities, and is a natural consequence of some current ideas about Population III star formation.
Abstract Copyright: 2005 The Authors. Journal compilation © 2005 RAS
Journal keyword(s): accretion, accretion discs - black hole physics - binaries: close - X-rays: binaries
CDS comments: HETE J1900.1-2455 = EQ J1900.1-2455.
Simbad objects: 5
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