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Are Q-stars a serious threat for stellar-mass black hole candidates
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Mon. Not. R. Astron. Soc. 000, 000–000 (0000) Printed 1 February 2008 (MN LATEX style file v1.4)
Are Q-stars a serious threat for stellar-mass black hole
candidates?
J.C. Miller,1,2 T. Shahbaz2 and L.A. Nolan2
1SISSA, via Beirut 2-4, 34013 Trieste, Italy
2Nuclear and Astrophysics Laboratory, University of Oxford, Keble Road, Oxford OX1 3RH
1 February 2008
ABSTRACT
We examine the status of the threat posed to stellar-mass black hole candidates by the
possible existence of Q-stars (compact objects with an exotic equation of state which
might have masses well above the normally-accepted maximum for standard neutron
stars). We point out that Q-stars could be extremely compact (with radii less than 1.5
times the corresponding Schwarzschild radius) making it quite difficult to determine
observationally that a given object is a black hole rather than a Q-star, unless there
is direct evidence for the absence of a solid surface. On the other hand, in order for
a Q-star to have a mass as high as that inferred for the widely-favoured black hole
candidate V404 Cygni, it would be necessary for the Q-matter equation of state to
apply already at densities an order of magnitude below that of nuclear matter and
this might well be considered implausible on physical grounds. We also describe how
rotation affects the situation and discuss the prospects for determining observationally
that black hole candidates are not Q-stars.
Key words: black hole physics – equation of state – binaries: close – X-rays: stars.
1 INTRODUCTION
The search for an unequivocal demonstration of the exis-
tence of stellar-mass black holes has focussed on X-ray emit-
ting binary systems consisting of an ordinary star together
with a compact object. If the mass of the compact object (as
determined from kinematical measurements) appears to be
greater than the maximum possible for a neutron starMmax,
then the object has been acknowledged as a bla
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