The plasma emission model of RX J1856.5-3754
1
Tbilisi State University, Chavchavadze Avenue 3, 0128 Tbilisi, Georgia e-mail: n.chkheidze@gmail.com
2
Abastumani Astrophysical Observatory, Al. Kazbegi Avenue 2a, 0160 Tbilisi, Georgia e-mail: g.machabeli@astro-ge.org
Received:
23
January
2007
Accepted:
15
May
2007
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 occur 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 estimated
Key words: stars: pulsars: individual: RX J1856.5-3754 / radiation mechanisms: non-thermal
© ESO, 2007