Magnetic fields generated by r-modes in accreting quark stars
We show that the r-mode instability can generate strong toroidal fields in the core of accreting millisecond quark stars by inducing differential rotation. We follow the spin frequency evolution on a long time-scale, taking into account the magnetic damping rate in the evolution equations of r-modes...
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| Hauptverfasser: | , , , , |
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| Dokumenttyp: | Article (Journal) |
| Sprache: | Englisch |
| Veröffentlicht: |
13 July 2011
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| In: |
Astronomy and astrophysics
Year: 2011, Jahrgang: 532, Pages: 1-7 |
| ISSN: | 1432-0746 |
| DOI: | 10.1051/0004-6361/201116661 |
| Online-Zugang: | Verlag, lizenzpflichtig, Volltext: https://doi.org/10.1051/0004-6361/201116661 Verlag, lizenzpflichtig, Volltext: https://www.aanda.org/articles/aa/abs/2011/08/aa16661-11/aa16661-11.html 
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| Verfasserangaben: | L. Bonanno, C. Cuofano, A. Drago, G. Pagliara, and J. Schaffner-Bielich |
| Zusammenfassung: | We show that the r-mode instability can generate strong toroidal fields in the core of accreting millisecond quark stars by inducing differential rotation. We follow the spin frequency evolution on a long time-scale, taking into account the magnetic damping rate in the evolution equations of r-modes. The maximum spin frequency of the star is only marginally lower than without the magnetic field. The late-time evolution of the stars that enter the r-mode instability region is instead quite different if the generated magnetic fields are taken into account: they leave the millisecond pulsar region and become radio pulsars. |
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| Beschreibung: | Gesehen am 06.04.2022 |
| Beschreibung: | Online Resource |
| ISSN: | 1432-0746 |
| DOI: | 10.1051/0004-6361/201116661 |