Abstract
view Abstract Citations (41) References (18) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Asymptotic freedom and dense stellar matter. II. The equation of state for neutron stars. Kislinger, M. B. ; Morley, P. D. Abstract The choice of the renormalization prescription used in the perturbative calculation of the quark-gluon thermodynamic potential and the quark mass parameter is discussed. It is shown that a judicious choice of subtraction points lumps all large logarithms into an effective, density-dependent, coupling constant whose value determines the validity of perturbation theory. The equation of state and the approach to nuclear densities are considered. The determination of the density above which the perturbation theory is valid requires the computation of the fully interacting equation of state. The thermodynamic potential is computed in this connection. The implications of the equation of state are examined. The stiffness above nuclear densities, followed by a softening at 7 x 10 to the 14th power g/cu cm, leads to moderately high neutron star masses. Publication: The Astrophysical Journal Pub Date: February 1978 DOI: 10.1086/155866 Bibcode: 1978ApJ...219.1017K Keywords: Astrophysics; Hadrons; Neutron Stars; Supernovae; Asymptotic Methods; Density (Mass/Volume); Equations Of State; Matter (Physics); Nuclear Reactions; Quarks; Astrophysics; Dense Matter; Neutron Stars full text sources ADS |
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