| Issue |
A&A
Volume 429, Number 3, January III 2005
|
|
|---|---|---|
| Page(s) | 999 - 1006 | |
| Section | Stellar structure and evolution | |
| DOI | https://doi.org/10.1051/0004-6361:20041442 | |
| Published online | 05 January 2005 | |
PSR B0809+74: Understanding its perplexing
subpulse-separation (P
) variations
1
Sterrenkundig Instituut “Anton Pannekoek”, 1098 SJ Amsterdam, The Netherlands e-mail: jrankin@astro.uva.nl; joanna.rankin@uvm.edu
2
Department of Astronomy, University of California, Berkeley, CA 94720, USA e-mail: ramach@astron.berkeley.edu
3
Pushchino Radioastronomy Observatory of the Lebedev Physical Institute, 142290, Russia e-mail: suleym@prao.psn.ru
4
Isaac Newton Institute of Chile, Pushchino Branch
Received:
9
June
2004
Accepted:
28
August
2004
The longitude separation between adjacent drifting subpulses, P2, is roughly constant for many pulsars. It was then perplexing when pulsar B0809+74 was found to exhibit substantial variations in this measure, both with wavelength and with longitude position within the pulse window. We analyze these variations between 40 and 1400 MHz, and we show that they stem primarily from the incoherent superposition of the two orthogonal modes of polarization.
Key words: stars: pulsars: general / polarisation / radiation machanisms: non-thermal
© ESO, 2005
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