Neutron Stars, Supernova Explosions and the Transition to Quark Matter

Details Neutron Stars, Supernova Explosions and the Transition to Quark Matter Neutron Stars, Supernova Explosions and the Transition to Quark Matter

Dec 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998tx19.confe.217d&link_type=abstract

Abstracts of the 19th Texas Symposium on Relativistic Astrophysics and Cosmology, held in Paris, France, Dec. 14-18, 1998. Eds.:

Astronomy and Astrophysics

Astrophysics

Scientific paper

The transition to quark matter can take place in neutron stars. The structure of a hybrid star, containing a core made of quark matter will be discussed. The maximum mass of the hybrid star turns out to be 1.59 M_odot. Possible signatures of the quark phase as pulsar's timing, cooling rate etc. will be considered. The deconfinement transition can also take place during the collapse of a supernova. A finite temperature EOS is introduced and its dependence on the proton fraction is shown to be crucial. The softening of the EOS at densities just above nuclear matter saturation density for Z/A ~0.3 helps in obtaining an explosion. At the same time, at larger densities the EOS is stiff enough to support a neutron star compatible with observations. A. Drago, U. Tambini, M. Hjorth-Jensen, Phys. Lett. B 380 (1996) 13; A. Drago and U. Tambini, astro-ph/9703138.

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