Volume 532, August 2011
|Number of page(s)||7|
|Section||Stellar structure and evolution|
|Published online||13 July 2011|
Magnetic fields generated by r-modes in accreting quark stars
Institut für Theoretische Physik, Ruprecht-Karls-Universität, Philosophenweg 16, 69120 Heidelberg, Germany
2 Dipartimento di Fisica, Universitá di Ferrara and INFN sezione di Ferrara, 44100 Ferrara, Italy
3 Institute for Theoretical Physics, Goethe University, Max-von-Laue-Str. 1, 60438 Frankfurt am Main, Germany
Received: 4 February 2011
Accepted: 29 May 2011
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.
Key words: X-rays: binaries / gravitational waves / magnetic fields / instabilities / pulsars: general
© ESO, 2011
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