Volume 465, Number 2, April II 2007
|Page(s)||575 - 586|
|Section||Stellar structure and evolution|
|Published online||29 January 2007|
The geometry of PSR B0031-07
Department of Astrophysics, Radboud University, Nijmegen, The Netherlands e-mail: Roy.Smits@manchester.ac.uk
2 National Center for Radio Astrophysics, Pune, India
3 ASTRON, Dwingeloo, The Netherlands
4 Astronomical Institute “Anton Pannekoek”, Amsterdam, The Netherlands
5 Max-Planck-Insitut für Radioastronomy, Bonn, Germany
Accepted: 20 January 2007
Context.PSR B0031-07 is well known to exhibit three different modes of drifting sub-pulses (mode A, B and C). It has recently been shown that in a multifrequency observation, consisting of 2700 pulses, all driftmodes were visible at low frequencies, while at 4.85 GHz only mode-A drift or non-drifting emission was detected. This suggests that modes A and B are emitted in sub-beams, rotating at a fixed distance from the magnetic axis, with the mode-B sub-beams being closer to the magnetic axis than the mode-A sub-beams. Diffuse emission between the sub-beams can account for the non-drifting emission.
Aims.Using the results of an analysis of simultaneous multifrequency observations of PSR B0031-07, we set out to construct a geometrical model that includes emission from both sub-beams and diffuse emission and describes the regions of the radio emission of PSR B0031-07 at each emission frequency for driftmodes A and B.
Methods.Based on the vertical spacing between driftbands, we have determined the driftmode of each sequence of drift. To restrict the model, we calculated average polarisation and intensity characteristics for each driftmode and at each frequency.
Results.The model reproduces the observed polarisation and intensity characteristics, suggesting that diffuse emission plays an important role in the emission properties of PSR B0031-07. The model further suggests that the emission heights of this pulsar range from a few kilometers to a little over 10 kilometers above the pulsar surface. We also find that the relationships between height and frequency of emission that follow from curvature radiation and from plasma-frequency emission could not be used to reproduce the observed frequency dependence of the width of the average intensity profiles.
Key words: stars: neutron / stars: pulsars: general / stars: pulsars: individual: PSR B0031-07
© ESO, 2007
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