Hostname: page-component-cd9895bd7-p9bg8 Total loading time: 0 Render date: 2024-12-24T01:49:53.342Z Has data issue: false hasContentIssue false
  • English
  • Français

Magnetic Fields in our Galaxy: How much do we Know? I. Disk fields within a few kpc of the Sun

Published online by Cambridge University Press:  12 April 2016

J.L. Han
J.L. Han*
Affiliation:
The Partner Group of MPlfR, National Astronomical Observatories of China, Jia-20 DaTun Rd., Chao Yang District, Beijing 100012, China. E-mail: [email protected]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The large scale magnetic fields of our Galaxy have been mostly revealed by rotation measures (RMs) of pulsars and extragalactic radio sources. In the disk of our Galaxy, the average field strength over a few kpc scale is about 1.8 μG, while the total field, including the random fields on smaller scales, has a strength of about 5 μG. The local regular field, if it is part of the large scale field of a bisymmetric form, has a pitch angle of about −8°. There are at least three, and perhaps five, field reversals from the Norma arm to the outer skirt of our Galaxy.

Type
Chapter Four Extreme Scattering Events, Distribution of Material and IPS
Information
International Astronomical Union Colloquium , Volume 182: Sources and Scintillations: Refraction and Scattering in Radio Astronomy , 2001 , pp. 181 - 184
Copyright
Copyright © Kluwer 2001

References

Andreasyan, R.R. and Makarov, A.N.: 1989, Astrofiz. 31(2), 247.Google Scholar
Beck, R., Brandenburg, A., Moss, D., Shukurov, A. and Sokoloff, D.: 1996, Annu. Rev. Astron. Astrophys. 34, 155.Google Scholar
Clegg, A.W., Cordes, J.M., Simonetti, J.H. and Kulkarni, S.R.: 1992, Astrophys. J. 386, 143.CrossRefGoogle Scholar
Hamilton, P.N. and Lyne, A.G.: 1987, Mon. Not. R. Astron. Soc. 224, 1073.Google Scholar
Han, J.L.: 2002, in Astmphysical Polarized Background, Cecchini, S., Cortiglioni, S., Sault, R. and Sbarra, C. (eds.), American Institute of Physics, in press.Google Scholar
Han, J.L., Manchester, R.N., Berkhuijsen, E.M. and Beck, R.: 1997, Astron. Astrophys. 322, 98.Google Scholar
Han, J.L., Manchester, R.N. and Qiao, G.J.: 1999a, Mon. Not. R. Astron. Soc. 306, 371 (HMQ99).Google Scholar
Han, J.L. and Qiao, G.J.: 1994, Astron. Astrophys. 288, 759 (HQ94).Google Scholar
Heiles, C.: 1996a, Astrophys. J. 462, 316.Google Scholar
Indrani, C. and Deshpande, A.A.: 1998, New Astron. 4, 33 (ID98).Google Scholar
Lyne, A.G. and Smith, K.G.: 1989, Mon. Not. R. Astron. Soc. 237, 533.Google Scholar
Manchester, R.N.: 1974, Astrophys. J. 188, 637.CrossRefGoogle Scholar
Mathewson, D.S. and Ford, V.L.: 1970, Mem. R. Astron. Soc. 74, 139.Google Scholar
Ohno, H. and Shibata, S.: 1993, Mon. Not. R. Astron. Soc. 262, 953.CrossRefGoogle Scholar
Rand, R.J., and Kulkarni, S.R.: 1989, Astrophys. J. 343, 760 (RK89).Google Scholar
Rand, R.J. and Lyne, A.G.: 1994, Mon. Not. R. Astron. Soc. 268, 497.Google Scholar
Simard-Normandin, M. and Kronberg, P.P.: 1980, Astrophys. J. 242, 74 (SK80).Google Scholar
Sofue, Y. and Fujimoto, M.: 1983, Astrophys. J. 265, 722 (SF83).Google Scholar
Thomson, R.C. and Nelson, A.H.: 1980, Mon. Not. R. Astron. Soc. 191, 863 (TN80).CrossRefGoogle Scholar
Vallée, J.P.: 1996, Astron. Astrophys. 308, 433.Google Scholar
Zweibel, E.G. and Heiles, C.: 1997, Nature 385, 131.Google Scholar