Thermal evolution of a pulsating neutron star
We have derived a set of equations to describe the thermal evolution of a neutron star which undergoes small-amplitude radial pulsations. We have taken into account, within the framework of the general theory of relativity, the pulsation damping due to the bulk and shear viscosity and the accompanyi...
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| Veröffentlicht in: | Monthly notices of the Royal Astronomical Society 2005-08, Vol.361 (4), p.1415-1424 |
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| container_title | Monthly notices of the Royal Astronomical Society |
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| creator | Gusakov, M. E. Yakovlev, D. G. Gnedin, O. Y. |
| description | We have derived a set of equations to describe the thermal evolution of a neutron star which undergoes small-amplitude radial pulsations. We have taken into account, within the framework of the general theory of relativity, the pulsation damping due to the bulk and shear viscosity and the accompanying heating of the star. The neutrino emission of a pulsating non-superfluid star and its heating due to the bulk viscosity are calculated assuming that both processes are determined by the non-equilibrium modified Urca process. Analytical and numerical solutions to the set of equations of the stellar evolution are obtained for linear and strongly non-linear deviations from beta-equilibrium. It is shown that a pulsating star may be heated to very high temperatures, while the pulsations damp very slowly with time as long as the damping is determined by the bulk viscosity (a power-law damping over 100–1000 yr). The contribution of the shear viscosity to the damping becomes important in a rather cool star with a low pulsation energy. |
| doi_str_mv | 10.1111/j.1365-2966.2005.09295.x |
| format | Article |
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It is shown that a pulsating star may be heated to very high temperatures, while the pulsations damp very slowly with time as long as the damping is determined by the bulk viscosity (a power-law damping over 100–1000 yr). The contribution of the shear viscosity to the damping becomes important in a rather cool star with a low pulsation energy.</description><identifier>ISSN: 0035-8711</identifier><identifier>EISSN: 1365-2966</identifier><identifier>DOI: 10.1111/j.1365-2966.2005.09295.x</identifier><language>eng</language><publisher>23 Ainslie Place, Edinburgh EH3 6AJ, UK. 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It is shown that a pulsating star may be heated to very high temperatures, while the pulsations damp very slowly with time as long as the damping is determined by the bulk viscosity (a power-law damping over 100–1000 yr). The contribution of the shear viscosity to the damping becomes important in a rather cool star with a low pulsation energy.</description><subject>Astronomy</subject><subject>Neutrons</subject><subject>Numerical analysis</subject><subject>Stars & galaxies</subject><subject>stars: evolution</subject><subject>stars: neutron</subject><subject>stars: oscillations</subject><subject>Thermal energy</subject><issn>0035-8711</issn><issn>1365-2966</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2005</creationdate><recordtype>article</recordtype><recordid>eNqNkEtPwzAMgCMEEmPwHyruLc57PXBAEzBgPDQGQlyitEugpWtH0sL272kp2hlfbNn-bOlDKMAQ4TZO8ghTwUMSCxERAB5BTGIerXfQYDvYRQMAysORxHgfHXifAwCjRAxQOH83bqmLwHxVRVNnVRlUNtDBqim8rrPyLShNU7u27WvtDtGe1YU3R395iJ4uzufjSTi9v7wan03DlJFR-wcLA9ZQyxbWQEIkNqkUOl5ICgIShiFJUhbzRIDAzDBLLCQ2pQvKdSrThA7RcX935arPxvha5VXjyvalIiApo4LwdmnUL6Wu8t4Zq1YuW2q3URhU50blqlOgOgWqc6N-3ah1i5726HdWmM2_OXV7N-uqlg97PvO1WW957T6UkFRyNXl5VRN5_fg8u3lQQH8AWGd5Iw</recordid><startdate>20050821</startdate><enddate>20050821</enddate><creator>Gusakov, M. 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| ispartof | Monthly notices of the Royal Astronomical Society, 2005-08, Vol.361 (4), p.1415-1424 |
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| language | eng |
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| source | Wiley Online Library - AutoHoldings Journals; Oxford Journals Open Access Collection |
| subjects | Astronomy Neutrons Numerical analysis Stars & galaxies stars: evolution stars: neutron stars: oscillations Thermal energy |
| title | Thermal evolution of a pulsating neutron star |
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