The internal structure of neutron stars and white dwarfs, and the Jacobi virial equation. II.
Context. The Jacobi virial equation is a very powerful tool for exploring several aspects of the stellar internal structure and evolution. In a previous paper we have shown that the function [αβ]GR Lambda0.9(R) is constant (≈0.4) for pre main-sequence stars (PMS), white dwarfs (WD) and for some neut...
| Autores: | , |
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| Tipo de recurso: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 2013 |
| País: | España |
| Institución: | Consejo Superior de Investigaciones Científicas (CSIC) |
| Repositorio: | DIGITAL.CSIC. Repositorio Institucional del CSIC |
| OAI Identifier: | oai:digital.csic.es:10261/405374 |
| Acceso en línea: | http://hdl.handle.net/10261/405374 |
| Access Level: | acceso abierto |
| Palabra clave: | Stars: evolution Stars: interiors Stars: neutron Stars: pre-main sequence White dwarfs |
| Sumario: | Context. The Jacobi virial equation is a very powerful tool for exploring several aspects of the stellar internal structure and evolution. In a previous paper we have shown that the function [αβ]GR Lambda0.9(R) is constant (≈0.4) for pre main-sequence stars (PMS), white dwarfs (WD) and for some neutron star (NS) models, where αGR and βGR are the form-factors of the gravitational potential energy and of the moment of inertia |
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