Plasma Turbulence as a Mechanism of Pulsar Radiation

Details Plasma Turbulence as a Mechanism of Pulsar Radiation Plasma Turbulence as a Mechanism of Pulsar Radiation

May 1970

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1970natur.226..731i&link_type=abstract

Nature, Volume 226, Issue 5247, pp. 731-733 (1970).

Computer Science

7

Scientific paper

RADIO signals from pulsars are characterized by (1) high intensity, with brightness temperatures of the order of 1021 K (ref. 1); (2) pronounced (mostly linear) polarizations with, in the case of PSR 0833 (ref. 2), a monotonic sweep of the polarization angle during each pulse; (3), narrow pulse widths (Δt) compared with the repetition period (P); and (4) optical, X-ray and radio pulse widths, which are virtually the same3. This report is about a pulsar model in which anisotropic plasma turbulence, produced by the onset of a two-stream instability near the light cylinder of a rotating magnetic star, is the chief radiation mechanism. The model offers a quantitative, self-consistent account of features (1)-(3) for quite different pulsars, and a qualitative explanation of feature (4).

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