2000/12/05 by R. Mańka, R. Manka, M. Zastawny-Kubica +4 · 1 citation
Earth and Planetary Sciences · Physics and Astronomy · #Gamma-ray bursts and supernovae #Geophysics and Gravity Measurements #Pulsars and Gravitational Waves Research #astro-ph
paper · pdf · doi:10.1088/0954-3899/27/9/304
21 pages, iop latex2e, 18 colour figures, submitted to Journal of Physics G: Nuclear and Particle
arxiv created 2000/12/05 · openalex publication_date 2001/08/03 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/30
In this paper the basic properties of non-rotating and slowly rotating protoneutron stars in the relativistic mean-field approach are discussed. The equation of state is the main input to the structure equations. The TM1 parameter set extended to the finite-temperature case is used to obtain the mass-radius relation for protoneutron stars. The occurrence of unstable branches in the mass-radius relation are presented. This allows for the existence of distinctively different evolution tracks for protoneutron stars. The low-density protoneutron star configurations are estimated. The stable configurations obtained for fixed lepton number Y L = 0.4 are compared with those obtained for fixed proton fraction Y P = 0.1776.