Volume 447, Number 1, February III 2006
|Page(s)||235 - 243|
|Section||Stellar structure and evolution|
|Published online||27 January 2006|
Phenomenology of pulsar B0809+74's rotating subbeam system
I. Geometry and profile “absorption”
Sterrenkundig Instituut “Anton Pannekoek”, 1098 SJ Amsterdam, The Netherlands e-mail: email@example.com, firstname.lastname@example.org
2 Department of Astronomy, University of California, Berkeley, CA 94720, USA e-mail: email@example.com
3 Pushchino Radio Astronomy Observatory, 142290 Pushchino, Russia e-mail: firstname.lastname@example.org
4 Isaac Newton Institute of Chile, Pushchino Branch
Accepted: 23 August 2005
The basic emission geometry of pulsar B0809+74 is modeled after determinating its polarization position-angle traverse. As the star's profiles are truncated by “absorption” over a broad band, most severely between some 60 and 1500 MHz, the analysis also provides quantitative estimates of the extent of this effect at each frequency. The model's predicted scales are found to agree closely with those determined by correlating pulse sequences observed simultaneously in different bands and by measuring P2 at different frequencies.
Key words: stars: pulsars: individual: B0809+74 / polarisation / radiation mechanisms: non-thermal
© ESO, 2006
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