Download Electrodynamics of paramagnetic neutron star

Post-burst pulsed X-ray and
gamma-ray emission of magnetars
(SGR & AXP) is most likely powered
by non-radial torsion oscillations of
neutron stars
Sergey Bastrukov
• Non-typically long period for young
neutron star
F. Weber
Global Torsional Pulsations
Magnetic field frozen in the neutron star
serves as a chief promoter of radiative
activity of pulsars magnetars
Alfven MHD pulsations of neutron
star in dissipative free regime
The detected QPO’s (periodicity) in X-ray emission of neutron stars can
be caused by non-radial Alfven MHD oscillations of neutron stars.
Torsional vibrations in the surface layers
may explain oscillations in the tail of
Type I X-ray bursts
T. Strohmayer &
A.Watts
Electromagnetic properties of
neutron star matter
The point is to compute periods of
Alfven oscillations in the crust
Oscillations of crust against core generating spiral
magneto-electron waves (helicons or whistlers)
Spiral oscillations of magnetic flux density and density
of electron flow in spiral magneto-electron wave
X-ray and gamma-ray emission can be
generated by cyclotron oscillations of electrons