Hostname: page-component-586b7cd67f-2plfb Total loading time: 0 Render date: 2024-11-30T04:35:38.131Z Has data issue: false hasContentIssue false
  • English
  • Français

The Magnetic Field in M33

Published online by Cambridge University Press:  19 July 2016

U.R. Buczilowski  and
R. Beck
U.R. Buczilowski
Affiliation:
Max-Planck-Institut für Radioastronomie Auf dem Hügel 69 D-5300 Bonn 1, F.R.G.
R. Beck
Affiliation:
Max-Planck-Institut für Radioastronomie Auf dem Hügel 69 D-5300 Bonn 1, F.R.G.

Extract

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.

Measurements at five radio wavelengths between 2.8 and 21.1 cm (Buczilowski and Beck, 1987) with the Effelsberg 100-m telescope make M33 the best studied nearby galaxy in linear polarization so far. The polarized emission is concentrated to the northwestern quadrant of the galaxy. Almost no polarization is detectable around the 35 known supernova remnant candidates. The explosions may have disturbed the interstellar magnetic field on scale sizes smaller than our antenna beams.

Type
5. The Polarization, Magnetic Field and Velocity Structure of External Spiral Galaxies
Information
Symposium - International Astronomical Union , Volume 140: Galactic and Intergalactic Magnetic Fields , 1990 , pp. 210
Copyright
Copyright © Kluwer 1990 

References

Buczilowski, U.R. and Beck, R. (1987), Astron. Astrophys. Suppl. 68, 171–185.Google Scholar
Tosa, M. and Fujimoto, M. (1978), Publ. Astron. Soc. Japan 30, 315–325.Google Scholar