Abstract
The gravitational wave, through the strongly magnetized plasma surrounding the neutron stars, in the [Formula: see text]-direction, deforms plasma particle rings in ellipses, alternating axes periodically along the direction of the magnetic field ([Formula: see text]-axis) and of the [Formula: see text]-axis. The uniform field leads to a modulation of the magnetic field, which results in magnetic pressure gradients (magneto-acoustic mode) or in the shear of the magnetic field lines (Alfvén mode). The gravitational wave drives MHD modes and transfers energy to the plasma, can become an important alternative process for the acceleration of baryons to high Lorentz factors observed in short GRBs. The total amount of energy that is transferred from the gravitational wave to the plasma is estimated ([Formula: see text]J - [Formula: see text] J), with [Formula: see text]. We compare our results with previously obtained results by other works.
Highlights
Binary systems that include Neutron Stars (NSs) are considered the most likely progenitors for short Gamma-Ray Bursts.[1]
The gravitational radiation produced by these compact stars travels through their heavily magnetized (∼ 1012 G) magnetospheres with density up to n ∼ 1012 cm−3, and indirectly interacts with the electromagnetic fields coupled to the matter
The mechanism of gravitational waves (GWs) energy deposition into the plasma, exciting MHD modes, may become an alternative process for GRB’s fireball ignition, such as it accelerates the baryonic matter to high Lorentz factors.[7]
Summary
Binary systems that include Neutron Stars (NSs) are considered the most likely progenitors for short Gamma-Ray Bursts (sGRBs).[1]. There are several types of astronomical objects that can produce significant amounts of gravitational waves (GWs) together with ultra relativistic free-force winds.[5] Coalescence of NSs (see Ref.5), for example, emits high frequency GW through the magnetosphere – composed by highly magnetized electron-positron plasma – of these objects. The gravitational radiation produced by these compact stars travels through their heavily magnetized (∼ 1012 G) magnetospheres with density up to n ∼ 1012 cm−3, and indirectly interacts with the electromagnetic fields coupled to the matter.
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