2006/07/26 by O. E. Nicotra, Nicotra, O. E.
Earth and Planetary Sciences · Physics and Astronomy · #Astrophysics (astro-ph) #FOS: Physical sciences #Geophysics and Gravity Measurements #High-pressure geophysics and materials #Nuclear Theory (nucl-th) #Pulsars and Gravitational Waves Research #astro-ph #nucl-th
paper · pdf · doi:10.48550/arxiv.nucl-th/0607055
5 pages, 3 figures, 1 table
openalex publication_date 2006/07/26 · arxiv created 2006/08/07 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
To investigate the stability of the protoneutron stars in their early evolution, the minimum gravitational mass plays a fundamental role. This quantity depends upon the temperature profile assumed. We study within a static approach the stability of a protoneutron star. In particular we focus on a suitable temperature profile suggested by dynamical calculations. We consider a protoneutron star as composed of an isothermal core and an isentropic outer part. To describe physical properties of the interior we employ a microscopically derived equation of state for nuclear matter. For the outer part we employ the Lattimer-Swesty equation of state. The global structure is studied. The assumed temperature profile turns out to give a range of stability which supports temperature values in line with those coming from dynamical calculations. The maximum mass instead depends only upon the equation of state employed.