Can stellar mass black holes be quark stars?

Abstract

We investigate the possibility that stellar mass black holes, with masses in the range of $3.8M_{\odot }$ and $6M_{\odot }$, respectively, could be in fact quark stars in the Color-Flavor-Locked (CFL) phase. Depending on the value of the gap parameter, rapidly rotating CFL quark stars can achieve much higher masses than standard neutron stars, thus making them possible stellar mass black hole candidates. Moreover, quark stars have a very low luminosity and a completely absorbing surface - the infalling matter on the surface of the quark star is converted into quark matter. A possibility of distinguishing CFL quark stars from stellar mass black holes could be through the study of thin accretion disks around rapidly rotating quark stars and Kerr type black holes, respectively. Furthermore, we show that the radiation properties of accretion disks around black holes and CFL quark stars are also very similar. However, strange stars exhibit a low luminosity, but high temperature bremsstrahlung spectrum, which, in combination with the emission properties of the accretion disk, may be the key signature to differentiate massive strange stars from black hole.

27 pages, 5 figures, accepted for publication in MNRAS

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• Distinguishing Brans-Dicke-Kerr type naked singularities and black holes with their thin disk electromagnetic radiation properties
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• Wormhole geometries supported by quark matter at ultra-high densities
• Constraints on vector unparticle physics from cosmic censorship
• Properties of compact objects in quadratic non-metricity gravity
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