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| Auteurs principaux: | , , , , |
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| Format: | Preprint |
| Publié: |
2024
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| Accès en ligne: | https://arxiv.org/abs/2409.01785 |
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| _version_ | 1866912390697713664 |
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| author | Kumar, Deepak Karan, Asit Verma, Anshuman Mishra, Hiranmaya Mallick, Ritam |
| author_facet | Kumar, Deepak Karan, Asit Verma, Anshuman Mishra, Hiranmaya Mallick, Ritam |
| contents | Neutron stars are usually assumed to be cold; however, in certain dynamical astrophysical scenarios such as newly born neutron stars or binary star mergers, the temperature effects play a non-negligible role. We systematically derive the equation of state at finite-temperature within a relativistic mean-field hadronic model applicable to such proto-neutron stars. The equation of state so derived considerably affects the mass-radius curve, thereby affecting the nonradial quadruple $f$-mode oscillation frequencies.} Temperature effectively makes the equation of state stiffer at relatively low and intermediate densities, thereby making the star less compact and flattening the mass-radius curve. The $f$-mode frequency for low and intermediate-mass neutron stars decreases with temperature and thus should be easier to detect. The universal relation (connecting $f$-mode frequency, mass, and radius) changes nonlinearly with temperature. The parameters defining the universal relation [$ωM = a(T) \left(\frac{M}{R}\right) + b(T)$] becomes temperature dependent with the coefficients following a parabolic relation with temperature. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2409_01785 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Modification of the universal relation between mass, radius and nonradial $f$-mode oscillation in proto-neutron stars Kumar, Deepak Karan, Asit Verma, Anshuman Mishra, Hiranmaya Mallick, Ritam High Energy Astrophysical Phenomena Neutron stars are usually assumed to be cold; however, in certain dynamical astrophysical scenarios such as newly born neutron stars or binary star mergers, the temperature effects play a non-negligible role. We systematically derive the equation of state at finite-temperature within a relativistic mean-field hadronic model applicable to such proto-neutron stars. The equation of state so derived considerably affects the mass-radius curve, thereby affecting the nonradial quadruple $f$-mode oscillation frequencies.} Temperature effectively makes the equation of state stiffer at relatively low and intermediate densities, thereby making the star less compact and flattening the mass-radius curve. The $f$-mode frequency for low and intermediate-mass neutron stars decreases with temperature and thus should be easier to detect. The universal relation (connecting $f$-mode frequency, mass, and radius) changes nonlinearly with temperature. The parameters defining the universal relation [$ωM = a(T) \left(\frac{M}{R}\right) + b(T)$] becomes temperature dependent with the coefficients following a parabolic relation with temperature. |
| title | Modification of the universal relation between mass, radius and nonradial $f$-mode oscillation in proto-neutron stars |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2409.01785 |