Early neutron stars and quark matter

Details Early neutron stars and quark matter Early neutron stars and quark matter

Mar 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988acaps...7..266l&link_type=abstract

(Acta Astrophysica Sinica, vol. 7, no. 4, 1987, p. 266-272) Chinese Astronomy and Astrophysics (ISSN 0275-1062), vol. 12, March

Physics

Early Stars, Matter (Physics), Neutron Stars, Quarks, Density (Mass/Volume), Equations Of State, Hot Stars, Phase Transformations, Stellar Cores, Stellar Temperature

Scientific paper

The existence of quark matter (QM) in hot early neutron stars is considered theoretically, using the method of Baym and Chin (1976) to calculate the pressure and density at the phase transition between neutron and quark matter for various temperatures. The results are presented in tables and graphs and discussed in detail. It is found that QM cores can exist whenever the temperature exceeds 10 to the 10th K, and that their radii increase with decreasing QM bag constant. The total energy emitted by a star during cooling is estimated as 10 to the 53rd erg, assuming conservation of baryon number.

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