Differential rotation in neutron stars at finite temperatures
IntroductionThis paper investigates the impact of differential rotation on the bulk properties and onset of rotational instabilities in neutron stars at finite temperatures up to 50 MeV.MethodsUtilizing the relativistic Brueckner-Hartree-Fock (RBHF) formalism in full Dirac space, the study construct...
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Frontiers Media S.A.
2024-10-01
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| Series: | Frontiers in Physics |
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| Online Access: | https://www.frontiersin.org/articles/10.3389/fphy.2024.1474615/full |
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| author | Delaney Farrell Fridolin Weber Fridolin Weber Rodrigo Negreiros Rodrigo Negreiros |
| author_facet | Delaney Farrell Fridolin Weber Fridolin Weber Rodrigo Negreiros Rodrigo Negreiros |
| author_sort | Delaney Farrell |
| collection | DOAJ |
| description | IntroductionThis paper investigates the impact of differential rotation on the bulk properties and onset of rotational instabilities in neutron stars at finite temperatures up to 50 MeV.MethodsUtilizing the relativistic Brueckner-Hartree-Fock (RBHF) formalism in full Dirac space, the study constructs equation of state (EOS) models for hot neutron star matter, including conditions relevant for high temperatures. These finite-temperature EOS models are applied to compute the bulk properties of differentially rotating neutron stars with varying structural deformations.ResultsThe findings demonstrate that the stability of these stars against bar-mode deformation, a key rotational instability, is only weakly dependent on temperature. Differential rotation significantly affects the maximum mass and radius of neutron stars, and the threshold for the onset of bar-mode instability shows minimal sensitivity to temperature changes within the examined range.DiscussionThese findings are crucial for interpreting observational data from neutron star mergers and other high-energy astrophysical events. The research underscores the necessity of incorporating differential rotation and finite temperature effects in neutron star models to predict their properties and stability accurately. |
| format | Article |
| id | doaj-art-d87fccfe6e7643d182079403697b2696 |
| institution | OA Journals |
| issn | 2296-424X |
| language | English |
| publishDate | 2024-10-01 |
| publisher | Frontiers Media S.A. |
| record_format | Article |
| series | Frontiers in Physics |
| spelling | doaj-art-d87fccfe6e7643d182079403697b26962025-08-20T02:08:42ZengFrontiers Media S.A.Frontiers in Physics2296-424X2024-10-011210.3389/fphy.2024.14746151474615Differential rotation in neutron stars at finite temperaturesDelaney Farrell0Fridolin Weber1Fridolin Weber2Rodrigo Negreiros3Rodrigo Negreiros4Department of Physics, San Diego State University, San Diego, CA, United StatesDepartment of Physics, San Diego State University, San Diego, CA, United StatesDepartment of Physics, University of California at San Diego, San Diego, CA, United StatesDepartment of Physics, Catholic Institute of Technology, Cambridge, MA, United StatesInstituto de Física, Universidade Federal Fluminense, Rio deJaneiro, BrazilIntroductionThis paper investigates the impact of differential rotation on the bulk properties and onset of rotational instabilities in neutron stars at finite temperatures up to 50 MeV.MethodsUtilizing the relativistic Brueckner-Hartree-Fock (RBHF) formalism in full Dirac space, the study constructs equation of state (EOS) models for hot neutron star matter, including conditions relevant for high temperatures. These finite-temperature EOS models are applied to compute the bulk properties of differentially rotating neutron stars with varying structural deformations.ResultsThe findings demonstrate that the stability of these stars against bar-mode deformation, a key rotational instability, is only weakly dependent on temperature. Differential rotation significantly affects the maximum mass and radius of neutron stars, and the threshold for the onset of bar-mode instability shows minimal sensitivity to temperature changes within the examined range.DiscussionThese findings are crucial for interpreting observational data from neutron star mergers and other high-energy astrophysical events. The research underscores the necessity of incorporating differential rotation and finite temperature effects in neutron star models to predict their properties and stability accurately.https://www.frontiersin.org/articles/10.3389/fphy.2024.1474615/fullneutron stardifferential rotationequation of statebrueckner-Hartree-Fockfinite temperature field theorybar mode instability |
| spellingShingle | Delaney Farrell Fridolin Weber Fridolin Weber Rodrigo Negreiros Rodrigo Negreiros Differential rotation in neutron stars at finite temperatures Frontiers in Physics neutron star differential rotation equation of state brueckner-Hartree-Fock finite temperature field theory bar mode instability |
| title | Differential rotation in neutron stars at finite temperatures |
| title_full | Differential rotation in neutron stars at finite temperatures |
| title_fullStr | Differential rotation in neutron stars at finite temperatures |
| title_full_unstemmed | Differential rotation in neutron stars at finite temperatures |
| title_short | Differential rotation in neutron stars at finite temperatures |
| title_sort | differential rotation in neutron stars at finite temperatures |
| topic | neutron star differential rotation equation of state brueckner-Hartree-Fock finite temperature field theory bar mode instability |
| url | https://www.frontiersin.org/articles/10.3389/fphy.2024.1474615/full |
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