Open AccessObservational constraints on the radio and γ‐ray emission regions of PSR B1055−52
Author(s) -
Wang H. G.,
Qiao G. J.,
Xu R. X.,
Liu Y.
Publication year - 2006
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1111/j.1365-2966.2005.09743.x
Subject(s) - physics , field line , magnetic field , polarization (electrochemistry) , astrophysics , position angle , linear polarization , radio frequency , optics , galaxy , telecommunications , laser , chemistry , quantum mechanics , computer science
Observational constraints on the radio and γ‐ray emission regions of PSR B1055−52 seen through our line of sight are presented by analysing the position angle curves of radio linear polarization and fitting the observed pulse widths of radio and γ‐ray pulses and the phase offsets between them. Aberration, retardation and magnetic field sweep back effects that can cause additional phase offset between the emissions from different locations are taken into account. The following conclusions are obtained. (i) The radio main pulse and γ‐ray pulses are emitted from the same pole, while the radio interpulse is emitted from the opposite pole. (ii) The interpulse emission region locates on the open field lines much closer to the magnetic axis than those of the main pulse, and the emission altitudes are higher than those of the main pulse. (iii) At each pole, there are probably two groups of field lines where radio emission is generated, of which the outer one consists of open field lines near (or including) the last open field lines and the inner one consists of open field lines from very near the magnetic pole to approximately the midway between the magnetic axis and the last open field lines. (iv) The γ‐ray pulse comes from inner open field lines rather than from the last open field lines, and the emission altitudes are beyond the null charge surface.