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Equation of state of dense matter and maximum mass of neutron stars

Published online by Cambridge University Press:  15 May 2003

C. Motch ,
J.-M. Hameury  and
P. Haensel
P. Haensel*
Affiliation:
N. Copernicus Astronomical Center, Bartycka 18, 00-718 Warszawa, Poland
*
haensel@camk.edu.pl
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Abstract

Theoretical models of the equation of state (EOS)of neutron-star matter (starting with the crustand ending at the densest region of the stellar core) are reviewed. Apart froma broad set of baryonic EOSs, strange quark matter, and even more exotic (abnormaland Q-matter) EOSs are considered. Results of calculations of Mmaxfor non-rotating neutron stars and exotic compact stars are reviewed, withparticular emphasis on the dependence on the dense-matter EOS. Rapid rotationincreases Mmax, and this effect is studied for both neutron stars and exoticstars. Theoretical results are then confronted with measurements of masses of neutronstars in binaries, and the consequences of such a confrontation and their possible impacton the theory of dense matter are discussed.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 7: Final Stages of Stellar Evolution , 2003 , pp. 249
Copyright
© EAS, EDP Sciences, 2003

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