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: | , |
|---|---|
| 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 |
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| dc.title.none.fl_str_mv |
The internal structure of neutron stars and white dwarfs, and the Jacobi virial equation. II. |
| title |
The internal structure of neutron stars and white dwarfs, and the Jacobi virial equation. II. |
| spellingShingle |
The internal structure of neutron stars and white dwarfs, and the Jacobi virial equation. II. Claret, Antonio Stars: evolution Stars: interiors Stars: neutron Stars: pre-main sequence White dwarfs |
| title_short |
The internal structure of neutron stars and white dwarfs, and the Jacobi virial equation. II. |
| title_full |
The internal structure of neutron stars and white dwarfs, and the Jacobi virial equation. II. |
| title_fullStr |
The internal structure of neutron stars and white dwarfs, and the Jacobi virial equation. II. |
| title_full_unstemmed |
The internal structure of neutron stars and white dwarfs, and the Jacobi virial equation. II. |
| title_sort |
The internal structure of neutron stars and white dwarfs, and the Jacobi virial equation. II. |
| dc.creator.none.fl_str_mv |
Claret, Antonio Hempel, M. |
| author |
Claret, Antonio |
| author_facet |
Claret, Antonio Hempel, M. |
| author_role |
author |
| author2 |
Hempel, M. |
| author2_role |
author |
| dc.contributor.none.fl_str_mv |
Ministerio de Educación y Ciencia (España) Swiss National Science Foundation Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72] |
| dc.subject.none.fl_str_mv |
Stars: evolution Stars: interiors Stars: neutron Stars: pre-main sequence White dwarfs |
| topic |
Stars: evolution Stars: interiors Stars: neutron Stars: pre-main sequence White dwarfs |
| description |
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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2013 |
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2013 2025 2025 |
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info:eu-repo/semantics/article http://purl.org/coar/resource_type/c_6501 Publisher's version info:eu-repo/semantics/publishedVersion |
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article |
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publishedVersion |
| dc.identifier.none.fl_str_mv |
http://hdl.handle.net/10261/405374 |
| url |
http://hdl.handle.net/10261/405374 |
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Inglés |
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Inglés |
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info:eu-repo/semantics/openAccess |
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openAccess |
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EDP Sciences |
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EDP Sciences |
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reponame:DIGITAL.CSIC. Repositorio Institucional del CSIC instname:Consejo Superior de Investigaciones Científicas (CSIC) |
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Consejo Superior de Investigaciones Científicas (CSIC) |
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DIGITAL.CSIC. Repositorio Institucional del CSIC |
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DIGITAL.CSIC. Repositorio Institucional del CSIC |
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1869418310151438336 |
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The internal structure of neutron stars and white dwarfs, and the Jacobi virial equation. II.Claret, AntonioHempel, M.Stars: evolutionStars: interiorsStars: neutronStars: pre-main sequenceWhite dwarfsContext. 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 inertiaAims. To investigate the structural evolution of another type of celestial bodies, we extend these calculations to gaseous planets. We also analyse the cases for which this function is not conserved during some stellar evolutionary phases. Concerning NS, we study the influence of the equation of state (EOS) on this function and refine the exponent of the auxiliary function Λ(R). We also present a macroscopic criterion of stability for these stars.Methods. Non-stop calculations from the PMS to the white dwarf cooling sequences were performed with the MESA code. The covered mass range was 0.1–1.7 M⊙. We used the same code to compute models for gaseous planets with masses between 0.1–50 MJ. Neutron star models were computed using two codes. The first one is a modified version of the NSCool/TOV subroutines. The second code is a plain TOV solver that allows one to use seven previously described EOS. The relativistic moment of inertia and gravitational potential energy were computed through a fourth-order Runge-Kutta method.Results. By analysing the internal structure of gaseous planets we show that the function [αβ]GR/Λ0.8(R) ≡ Γ(M,EOS) is conserved for all models during the whole planetary evolution and is independent of the planet mass. For the PMS to the white dwarf cooling sequences, we have found a connection between the strong variations of Γ(M,EOS) during the intermediary evolutionary phases and the specific nuclear power. A threshold for the specific nuclear power was found. Below this limit this function is invariant (≈0.4) for these models, i.e., at the initial and final stages (PMS and WD). For NS, we showed that the function Γ(M,EOS) is also invariant (≈0.4) and is independent of the EOS and of the stellar mass. Therefore, we confirm that regardless of the final products of the stellar evolution, NS or WD, they recover the initial value of Γ(M,EOS) ≈ 0.4 acquired at the PMS. Finally, we have introduced a macroscopic stability criterion for NS models based on the properties of the relativistic product [αβ]GR.We thank the anonymous referee for his/her useful comments and suggestions. We would like to thank B. Rufino and V. Costa for their comments. The Spanish MEC (AYA2009-10394, AYA2009-14000-C03-01) is gratefully acknowledged for its support during the development of this work. M.H. acknowledges support from the High Performance and High Productivity Computing (HP2C) project, and the Swiss National Science Foundation (SNF) under project number no. 200020-132816/1. M.H. is also grateful for support from ENSAR/THEXO and CompStar, a research networking program of the ESF. This research has made use of the SIMBAD database, operated at the CDS, Strasbourg, France, and of NASA\u2019s Astrophysics Data System Abstract Service.Peer reviewedEDP SciencesMinisterio de Educación y Ciencia (España)Swiss National Science FoundationConsejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]202520252013info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionhttp://hdl.handle.net/10261/405374reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Inglés#PLACEHOLDER_PARENT_METADATA_VALUE##PLACEHOLDER_PARENT_METADATA_VALUE#info:eu-repo/grantAgreement/MICINN//AYA2009-10394info:eu-repo/grantAgreement/MICINN//AYA2009-14000-C03-01http://dx.doi.org/10.1051/0004-6361/201220565Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/4053742026-05-22T06:33:51Z |
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15,811543 |