Synchrotron Spectra of Short-Period Pulsars

Details Synchrotron Spectra of Short-Period Pulsars Synchrotron Spectra of Short-Period Pulsars

Feb 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001arep...45..138m&link_type=abstract

Astronomy Reports, Volume 45, Issue 2, February 2001, pp.138-143

Astronomy and Astrophysics

Astronomy

1

Scientific paper

A model with synchrotron radiation near the light cylinder is proposed to explain the observed spectra of short-period pulsars (P≤0.1 s). These spectra can be described if a power-law energy distribution of the emitting electrons with exponent γ=2 8 is assumed. For most pulsars, the peak frequency νm is below 10 MHz. The νm(γ) dependence is derived, and shows that the peak frequencies for pulsars with spectral indices α<1.5 may fall in the observable range. In particular, νm may be νm ˜ 100 MHz for PSR J0751 + 1807 and PSR J1640 + 2224. The observed radio spectrum of Geminga (PSR J0633 + 1746) can be described by a synchrotron model with a monoenergetic or Maxwellian distribution of relativistic electrons and a small angle β between the spin axis and magnetic moment (β ˜ 10°).

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