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L. A. Nowakowski (Dept. of Physics, UPR), N. D. R. Bhat (MIT Haystack Observatory), D. R. Lorimer (Jodrell Bank Observatory)
The upgraded Arecibo, along with the new facility pulsar backend, the Wideband Arecibo Pulsar Processor (WAPP), opened up new avenues for carrying out single-pulse studies of unprecedented quality. Our detailed analysis of some of the most recent data (at 1175 MHz) on PSR B0950+08, a bright, well-known pulsar, has led to several new and interesting results. As is well known, its profile is characterized by a main pulse (MP) and an inter pulse (IP). Our observations show that the main pulse is comprised of three components; the third component dominates the stronger pulses, while the weaker pulses are dominated by the second component. The structure of the IP is clearly double, and is in agreement with data from pre-upgrade Arecibo observations. Additionally, there is evidence for a new, third component (possibly double) that seems most prominent in weaker pulses, wherein there is only a weak trace of the other two components. The bridge of emission between the main pulse and the inter pulse is observed to be fairly stable in its strength, and is most prominent in weaker pulses. Further, our analysis of intensity dependence of individual pulses suggest a possible correlation between the intensities and locations of the inter pulse with the first (leading) component of the main pulse. We discuss the implications of the results for the emission geometry of the pulsar, specifically, for the two different models that have been postulated, viz., a nearly orthogonal rotator and the aligned rotator.
The author(s) of this abstract have provided an email address for comments about the abstract: leszekan@coqui.net
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Bulletin of the American Astronomical Society, 34, #4
© 2002. The American Astronomical Soceity.