Propagation and Transmission of Alfven Waves in Rotating Magnetars
arXiv:astro-ph/0406572 · doi:10.1086/423706
Abstract
We study the propagation and transmission of Alfven waves in the context of cylindrical geometry. This approximates the polar cap region of aligned pulsar with strong magnetic fields. Non-propagating region appears in the presence of rotation. The displacement current further prevents the low frequency modes from propagating near the stellar surface. The transmission rates to the exterior through the surface are calculated. The rates increase with the frequency and the magnetic field strength. The transmission also depends on the helicity states of the waves, but the difference becomes small in the high frequency regime. We also point out the possibility of the spin-up by outgoing wave emission in the low frequency regime, if a certain condition holds.
arXiv comment16 pages, 3 figures, Accepted in ApJ
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Cited by in corpus (5)
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- Electromagnetic fields in the exterior of an oscillating relativistic star -- II. Electromagnetic damping
- The Evolution of High Temperature Plasma in Magnetar Magnetospheres and its Implications for Giant Flares
- Model on pulsed GeV radiation from magnetars
- Behavior of Torsional Alfven Waves and Field Line Resonance on Rotating Magnetars