Intensity dependence of the PSR 0329 + 54 pulse profile

Details Intensity dependence of the PSR 0329 + 54 pulse profile Intensity dependence of the PSR 0329 + 54 pulse profile

Mar 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...269..325m&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 269, no. 1-2, p. 325-329.

Astronomy and Astrophysics

Astrophysics

4

Pulsars, Pulse Duration, Very Large Array (Vla), Pair Production, Radio Emission

Scientific paper

Following the analysis by Krishnamohan and Downs (1980) of the Vela pulsar, the behavior of the core and out-rider components of PSR 0329 + 54 is investigated by computing intensity dependent pulse profiles. VLA observations of individual pulses from PSR 0329 + 54 at 1415 MHz are used in the analysis. The most striking result of the analysis is core component arrival times are earlier for the more intense pulse profiles. The intensity dependent pulse profiles are interpreted in terms of the Cheng and Ruderman (1980) ion outflow model as (1) the change in emission heights of individual components due to the regulation of pair-production by the outflow of ions from the stellar surface or (2) the relocation of the core component excitation region due to localized heating of the stellar surface by energetic electrons. Interpretation (1) suggests that the core component emission height varies by roughly 280 km in the pulsar's magnetosphere while interpretation (2) suggests that the core component excitation region moves by no more than 43 m on the stellar surface. The intensity dependent profiles reflect some of the properties of pulsar mode-changing.

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