Microstructure of Pulsar Radio Pulses Measured with a Time Resolution of 62.5 ns at 1650 MHz

Details Microstructure of Pulsar Radio Pulses Measured with a Time Resolution of 62.5 ns at 1650 MHz Microstructure of Pulsar Radio Pulses Measured with a Time Resolution of 62.5 ns at 1650 MHz

Mar 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002arep...46..206p&link_type=abstract

Astronomy Reports, Volume 46, Issue 3, March 2002, pp.206-215

Astronomy and Astrophysics

Astronomy

3

Scientific paper

We present an analysis of pulsar observations carried out on two frequency channels at 1634 MHz and 1650 MHz with a time resolution of 62.5 ns on the 70-m radio telescope of the NASA Deep Space Network in Tidbinbilla. The data were recorded using the S2 system, intended primarily for VLBI observations. Microstructure with characteristic timescales of 270, 80, and 150 µs was detected in pulsars B0833-45, B1749-28, and B1933 + 16, respectively. The distribution of microstructure timescales for the Vela pulsar (B0833-45) is characterized by a gradual growth with decreasing timescale to 200 µs; the distribution has a maximum at 20 200 µs and falls off sharply for timescales below 20 µs. The statistical relation between the microstructure modulation index m and the corresponding timescale τ µ can be approximated by the power law dependence R∝τ &sun; 0.5 ; i.e., the intensity is higher for micropulses with longer durations. This contradicts the predictions of nonlinear models for the formation of micropulses by supercompact soliton wave packets. In all the pulsars studied, the time delays of the micropulses between the two frequency channels deviate from the expected dispersion laws for the interstellar plasma. In particular, the micropulses in the low-frequency channel arrive earlier than predicted by the dispersion measures derived previously from the mean pulse profiles. The deviation from the dispersion delay is determined most accurately for B0833-45, and is 4.9±0.2 µs. Such anomalous delays are probably associated with the effects of propagation of the radio emission within the pulsar magnetosphere.

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