The Plasma Emission Model of RX J1856.5-3754

Abstract

A spectral analysis of the nearby isolated neutron star RX J1856.5-3754 is presented. Applying the kinetic approach, the distribution functions of emitting electrons are derived and the entire spectra is fitted. It is found that waves excited by the cyclotron mechanism, come in the radio domain. We confirm that the cyclotron instability is quite efficient, since the estimations show that the time of wave-particle interaction is long enough for particles to acquire perpendicular momentum and generate observed radiation. The lack of rotational modulation is discussed and the pulsar spin period is estimated.

arXiv comment5 pages, 4 figures

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• On the emission polarization of RX J1856.5-3754
• On the mechanism of the pulsed high energy emission from the pulsar PSR B1509-58
• The plasma emission model of RBS1774