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Astron. Astrophys. 328, 409-418

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Neutrino synchrotron emission from dense magnetized electron gas of neutron stars

V.G. Bezchastnov1, P. Haensel2, A.D. Kaminker1, and D.G. Yakovlev1

1A.F. Ioffe Physical Technical Institute, 194021 St. Petersburg, Russia
2N. Copernicus Astronomical Center, Polish Academy of Sciences, Bartycka 18, PL-00716 Warszawa, Poland

Received 14 March 1997 / Accepted 24 July 1997


We study the synchrotron emission of neutrino pairs by relativistic, degenerate electrons in strong magnetic fields. Particular attention is paid to the case in which the dominant contribution comes from one or several lowest cyclotron harmonics. Calculations are performed using the exact quantum formalism and the quasiclassical approach. Simple analytic fits to the neutrino synchrotron emissivity are obtained in the domain of magnetized, degenerate and relativistic electron gas provided the electrons populate either many Landau levels or the ground level alone. The significance of the neutrino synchrotron energy losses in the interiors of cooling neutron stars is discussed.

Key words: dense matter - stars: interiors - stars: neutron - radiation mechnisms: non-thermal

Send offprint requests to: P. Haensel

© European Southern Observatory (ESO) 1997

Online publication: October 30, 1997
Last change: March 24, 1998