Analytical solution to the problem of interaction between a shock wave and a neutron star’s magnetosphereстатья

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Дата последнего поиска статьи во внешних источниках: 5 декабря 2014 г.

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[1] Bezrodnykh S. I., Somov B. V. Analytical solution to the problem of interaction between a shock wave and a neutron star’s magnetosphere // Doklady Physics. — 2014. — Vol. 59, no. 8. — P. 355–359. Neutron stars have magnetic fields the intensities of which can reach $1012-1015$ G. Such a strong magnetic field is responsible for the occurrence of some striking observable effects: directional relativistic plasma jets, particle acceleration to giant energies, and bursts of hard electromagnetic radiation. The study of the magnetospheres of neutron stars is a topical astrophysical problem. One of the important questions of this subject is the study of interaction between a shock wave from a supernova explosion and the magnetic field of a neutron star. This interaction produces a magnetosphere the boundary of which is determined by the equality of gas pressure p of the incident plasma flux and pressure of the magnetic field filling the circumstellar space. A reconnecting current layer forms in the magnetosphere’s tail, in which magnetic energy is released. The magnetic force B × curlB dominates over the gas pressure gradient, gravitational, and other forces up to appreciable distances from the star to the magnetosphere’s boundary. In this connection, a strong field approximation can be applied to describe the magnetohydrodynamic processes in the magnetosphere. In this work, an analytical solution to the problem of the magnetospheric boundary shape of a neutron star (which is a priori unknown) is constructed in the 2D stationary model and an explicit representation for the magnetic field is given. It is supposed in the considered model that the stellar magnetic field is approximated by a point dipole and a plane neutral current layer is located in the magnetospheric tail. These problems allowing for free boundaries have been studied in connection with astrophysical applica tions by many researchers for a long time. However, no solutions seem to have been obtained in a closed analytical form for models with current layers. [ DOI ]

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