We propose a model to explain how a Gamma Rays Burst. can take place days or years after a supenova explosion. Our model is based on the conversion of a pure hadronic star (neutron star) into a star made at least in part of deconfined quark matter. The conversion process can be delayed if the surface tension at the interface between hadronic and deconfined-quark-matter phases is taken into account. The nucleation time (i.e. the time to form a critical-size drop of quark matter) can be extremely long if the mass of the star is small. Via mass accretion the nucleation time can be dramaticaly reduced and the star is finally converted into the stable configuration. A huge amount of energy, of the order of 10(52)-10(53) erg, is released during the stellar conversion and can produce a powerful Gamma Ray Burst. The delay between the supemova explosion generating the metastable neutron star and the new collapse can explain the delay proposed in GRB990705 and in GRB011211
Quark matter formation in neutron stars and implications for gamma-ray bursts
BOMBACI, IGNAZIO;
2002-01-01
Abstract
We propose a model to explain how a Gamma Rays Burst. can take place days or years after a supenova explosion. Our model is based on the conversion of a pure hadronic star (neutron star) into a star made at least in part of deconfined quark matter. The conversion process can be delayed if the surface tension at the interface between hadronic and deconfined-quark-matter phases is taken into account. The nucleation time (i.e. the time to form a critical-size drop of quark matter) can be extremely long if the mass of the star is small. Via mass accretion the nucleation time can be dramaticaly reduced and the star is finally converted into the stable configuration. A huge amount of energy, of the order of 10(52)-10(53) erg, is released during the stellar conversion and can produce a powerful Gamma Ray Burst. The delay between the supemova explosion generating the metastable neutron star and the new collapse can explain the delay proposed in GRB990705 and in GRB011211I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
