Numerical models for superfluid neutron stars and application to pulsar glitches
| Autor: | Aurélien Sourie, Jérôme Novak, Micaela Oertel |
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| Přispěvatelé: | Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS) |
| Jazyk: | angličtina |
| Rok vydání: | 2018 |
| Předmět: | |
| Zdroj: | The Fourteenth Marcel Grossmann Meeting On Recent Developments in Theoretical and Experimental General Relativity, Astrophysics, and Relativistic Field Theories. World Scientific Publishing Co. Pte. Ltd. 14th Marcel Grossmann Meeting on Recent Developments in Theoretical and Experimental General Relativity, Astrophysics, and Relativistic Field Theories 14th Marcel Grossmann Meeting on Recent Developments in Theoretical and Experimental General Relativity, Astrophysics, and Relativistic Field Theories, Jul 2015, Rome, Italy. pp.4125-4130, ⟨10.1142/9789813226609_0551⟩ |
| DOI: | 10.1142/9789813226609_0551⟩ |
| Popis: | International audience; We describe recent progress in the modelling of realistic equilibrium configurations of rotating superfluid neutron stars, in a fully general relativistic framework. We compute stationary and axisymmetric configurations of neutron stars composed of two interpenetrating and interacting fluids, namely superfluid neutrons and charged particles (protons and electrons), rotating with different rotation rates around a common axis. Two different realistic equations of state are considered. As a first application, we propose a simple bulk model for pulsar glitches, seen as angular momentum transfers between the two fluids through mutual friction force. From a series of equilibrium states, we compute the evolution in time of the properties of a neutron star during the rise period of a glitch. This enables us to infer characteristic features relative to glitches, such as spin-up timescales, that could be compared with future accurate observations in order to put some constraints on the interior of neutron stars. |
| Databáze: | OpenAIRE |
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