The difference of the magnetic field of PSR 1133 + 16 from a dipole one

Details The difference of the magnetic field of PSR 1133 + 16 from a dipole one The difference of the magnetic field of PSR 1133 + 16 from a dipole one

Sep 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991pazh...17..797s&link_type=abstract

Pis'ma v Astronomicheskii Zhurnal (ISSN 0320-0108), vol. 17, Sept. 1991, p. 797-802. In Russian. In Russian. In Russian.

Astronomy and Astrophysics

Astronomy

1

Magnetic Dipoles, Pulsars, Stellar Magnetic Fields, Cross Correlation, Frequency Distribution, Radio Astronomy

Scientific paper

Simultaneous three-frequency high-resolution observations of PSR 1133 + 16 show that the use of the micropulse phase as a reference point for measuring the subpulse dispacement at different frequences makes it possible to define the magnetic field's structure. It is concluded that, at heights where emission occurs in the range 67.5-102.5 MHz, the magnetic field is not dipolar and the emission cone is curved in the direction of the tail component of the mean profile.

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