Quark-Nova

Abstract

We explore the scenario where the core of a neutron star (having experienced a transition to an up and down quark phase) shrinks into the equilibrated quark object after reaching strange quark matter saturation density (where a composition of up, down and strange quarks is the favored state of matter). The overlaying (envelope) material free-falls following the core contraction releasing upto 10^{53} {\rm ergs} in energy as radiation, partly as a result of the conversion of envelope material to quarks. This phenomena, we named Quark-Nova, leads to a wide variety of ejectae ranging form the Newtonian, "dirty" to the ultra-relativistic fireball. The mass range of the corresponding compact remnant (the quark star) ranges from less than 0.3M_{\odot} up to a solar mass. We discuss the connection between Quark-Novae and Gamma ray bursts and suggest the recently studied GRB011211 event as a plausible Quark-Nova candidate.

4 pages, 2 figures, shortened title. Major changes in the text, version to appear in Astronomy&Astrophysics

References in corpus (3)

• The Signature of Supernova Ejecta Measured in the X-ray Afterglow of Gamma-Ray Burst 011211
• Quark Stars as inner engines for Gamma Ray Bursts?
• The Glueball sector of two-flavor Color Superconductivity

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• Meissner Effect and Vortex Dynamics in Quark Stars -- A Model for Soft Gamma-Ray Repeaters
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