On the possibility of stable neutron stars in a unified description of quark-hadron matter.

Details On the possibility of stable neutron stars in a unified description of quark-hadron matter. On the possibility of stable neutron stars in a unified description of quark-hadron matter.

Oct 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990svjnp..52..675b&link_type=abstract

Sov. J. Nucl. Phys., Vol. 52, No. 4, p. 675 - 678

Physics

3

Neutron Stars

Scientific paper

The quark-hadron phase transition in nuclear matter at zero temperature is described in a potential model using the Hartree-Fock cluster approach. The stiffness and asymmetry energy of the nuclear matter are consequences of the Pauli principle for the nucleon constituents. The region of coexistence of quark and neutron matter covers the range (2.3 - 3.1) ρ0. By integrating the Tolman-Oppenheimer-Volkov equations the authors obtain a stable branch of a neutron star with maximum mass 2.2 Msun and radius of the quark core ≡3 km.

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