Evidence for a hard equation of state in the cores of neutron stars
| dc.creator | Vuille, Chris | |
| dc.date | 2008-12-19 | |
| dc.date.accessioned | 2026-07-07T12:20:54Z | |
| dc.date.available | 2026-07-07T12:20:54Z | |
| dc.description | The equation of state for matter with energy density above 2 x10^14 g/cm^3 is parametrized by P = kN^Gamma, where N is the number density, Gamma is the adiabatic index, and k a constant. Using this scheme to generate thousands of models, together with data on neutron star masses, it is found, for a core region with a constant adiabatic index, that the central density must satisfy 10^15 gm/cm^3 < rho_c < 10^16 gm/cm^3, with Gamma > 2.2. Further preliminary results indicate, based on the observed neutrino flux from supernova 1987a, that this number must be considerably higher, on the order of 3.5. These results provide evidence for a hard equation of state in the cores of neutron stars. | |
| dc.description | original figures and tables are no longer available | |
| dc.identifier | https://arxiv.org/abs/0812.3828 | |
| dc.identifier | http://arxiv.org/abs/0812.3828 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/213204 | |
| dc.subject | Astrophysics | |
| dc.title | Evidence for a hard equation of state in the cores of neutron stars | |
| dc.type | text |