Secular effects in the r-mode instability and generation of magnetic fields

Details Secular effects in the r-mode instability and generation of magnetic fields Secular effects in the r-mode instability and generation of magnetic fields

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001ragt.meet..103r&link_type=abstract

In Proceedings of RAGtime 2/3 Workshops on black holes and neutron stars, 11-13/8-10 October 2000/2001, Eds: S. Hledík and Z. St

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Scientific paper

The instability of r-mode oscillations in rapidly rotating neutron stars has been so far a source of surprises. The analyses carried to date have revealed the surprising existence of this instability and, perhaps even more surprisingly, have shown that such instability has a rather large parameter space in which it can survive against the damping produced by shear and bulk viscosity, as well as against the interaction with a solid star crust. The magnetohydrodynamic coupling of the modes with a stellar magnetic field, which is likely to be present, has recently been shown to provide another surprising aspect of the instability. We here review the relevance of a stellar magnetic field, its modifications under the action of the r-mode instability, and how the interaction between r-mode oscillations and a magnetic field should limit the onset and duration of the instability.

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