Selfconsistent Numerical Calculation of Relativistic Neutron Star Magnetospheres

Peter Biltzinger; Klaus Oswald Thielheim

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Selfconsistent Numerical Calculation of Relativistic Neutron Star Magnetospheres

Peter Biltzinger·Klaus Oswald Thielheim

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Abstract

Selfconsistent magnetospheres of rotating cosmic magnets (neutron stars/pulsars) with arbitrary inclination of the magnetic against the rotation axis are considered. Present studies concentrate on the regime dominated by the force--free surface (FFS). A macroscopic fluid description is applied and radiation reaction is taken into account. As in earlier work of our group, a 'standard set of parameters' is used. Under these conditions, the following features are found among other results: global charge separation exists for all degrees of inclination of the magnetic against the rotation axis; clouds of different charge are seperated by regions of vanishing particle number density; as expected, test particles inserted into the latter regions propagate into one of the adjacent clouds; strong polodial currents exist; locally averaged particle energies for protons typically range up to $10^{16}-10^{17}$ eV, depending on the angle of inclination.

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Peter Biltzinger, Klaus Oswald Thielheim. 2004-11-28. Selfconsistent Numerical Calculation of Relativistic Neutron Star Magnetospheres. https://arxiv.org/abs/astro-ph/0011306

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