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Structure of the Local Galactic Magnetic Field

Published online by Cambridge University Press:  19 July 2016

R. J. Rand  and
S. R. Kulkarni
R. J. Rand
Affiliation:
California Institute of Technology, 105-24 Pasadena, CA 91125
S. R. Kulkarni
Affiliation:
California Institute of Technology, 105-24 Pasadena, CA 91125

Abstract

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We have modeled the local Galactic magnetic field using pulsar rotation measures (RMs), of which there are now about 200 available. The North Polar Spur has a significant effect on pulsar RMs. Using RMs of 116 pulsars nearer than 3 kpc, we find that the local field has a strength B0 = 1.6 ± 0.2 μG toward longitude lB =96° ± 4°, with a reversal of the field at a distance Dr = 600 ± 80 pc toward the inner Galaxy. Relaxing the 3 kpc distance restriction, we find that a concentric ring model with reversals is superior to a bisymmetric spiral model as a fit to the data.

Type
2. The Magnetic Field Structure of the Milky Way: The Meeting of Observation and Theory
Information
Symposium - International Astronomical Union , Volume 140: Galactic and Intergalactic Magnetic Fields , 1990 , pp. 44 - 46
Copyright
Copyright © Kluwer 1990 

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