Structure of protoneutron stars within a static approach
| dc.creator | Nicotra, O. E. | |
| dc.date | 2006-07-26 | |
| dc.date | 2006-08-07 | |
| dc.date.accessioned | 2026-07-07T07:22:32Z | |
| dc.date.available | 2026-07-07T07:22:32Z | |
| dc.description | 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. | |
| dc.description | 5 pages, 3 figures, 1 table | |
| dc.identifier | https://arxiv.org/abs/nucl-th/0607055 | |
| dc.identifier | http://arxiv.org/abs/nucl-th/0607055 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/115690 | |
| dc.subject | Nuclear Theory | |
| dc.subject | Astrophysics | |
| dc.title | Structure of protoneutron stars within a static approach | |
| dc.type | text |