Phases of Dense Matter in Supernovae and Neutron Stars

SHEN Hong (申虹); WANG Yannan (王延楠)

doi:10.1088/1009-0630/14/7/03

Plasma Science and Technology > 2012 > 14(7): 581-584. > DOI: 10.1088/1009-0630/14/7/03

SHEN Hong (申虹), WANG Yannan (王延楠). Phases of Dense Matter in Supernovae and Neutron Stars[J]. Plasma Science and Technology, 2012, 14(7): 581-584. DOI: 10.1088/1009-0630/14/7/03

Citation:

SHEN Hong (申虹), WANG Yannan (王延楠). Phases of Dense Matter in Supernovae and Neutron Stars[J]. Plasma Science and Technology, 2012, 14(7): 581-584. DOI: 10.1088/1009-0630/14/7/03

Citation:

SHEN Hong (申虹), WANG Yannan (王延楠). Phases of Dense Matter in Supernovae and Neutron Stars[J]. Plasma Science and Technology, 2012, 14(7): 581-584. DOI: 10.1088/1009-0630/14/7/03

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Phases of Dense Matter in Supernovae and Neutron Stars

School of Physics, Nankai University, Tianjin 300071, China

Funds: supported by National Natural Science Foundation of China (Nos.\,10675064, 11075082)

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Received Date: May 16, 2011

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Abstract

Abstract

We study the properties of dense matter at finite temperature with various proton fractions for use in supernova simulations. The relativistic mean-field theory is used to describe homogeneous nuclear matter, while the Thomas-Fermi approximation is adopted to describe inhomogeneous matter. We also discuss the equation of state of neutron star matter at zero temperature in a wide density range. The equation of state at high densities can be significantly softened by the inclusion of hyperons.
- relativistic mean-field theory,
- equation of state, supernova,
- neutron star

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