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Correlation Between Galactic Non-Thermal Continuum Emission and HI-Column Density

Published online by Cambridge University Press:  19 July 2016

K. Beuermann  and
Y.G. Kim
K. Beuermann
Affiliation:
Institut für Astronomie und Astrophysik Technische Universität Berlin, PN 8-1 Hardenbergstr. 36 D-1000 Berlin 21
Y.G. Kim
Affiliation:
Institut für Astronomie und Astrophysik Technische Universität Berlin, PN 8-1 Hardenbergstr. 36 D-1000 Berlin 21

Extract

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The distribution of magnetic field strengths in the interstellar gas is an important datum which relates to the formation of dense cloud complexes as well as to the distribution and propagation of cosmic rays. Brown and Chang (1983) found the brightness temperature of the radio continuum emission to be correlated with the HI column density NH and deduced a field strength which increases with particle density as <H> ~ <n>0.44. Troland and Heiles (1986) critized their approach and pointed out that Zeeman measurements suggest no increase in field strength for particle densities n ≤ 100 H-atoms cm-3.

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. 59 - 60
Copyright
Copyright © Kluwer 1990 

References

Beuermann, K., Kanbach, G., Berkhuijsen, E.M.: 1985, Astron. Astrophys. 153, 17 Google Scholar
Brown, R.L., Chang, C.-A.: 1983, Astrophys. J. 264, 134 CrossRefGoogle Scholar
Haslam, C.G.T., Salter, C.J., Stoffel, H., Wilson, W.E.: 1981, Astron. Astrophy. Suppl. 47, 1 Google Scholar
Troland, T.H., Heiles, C.: 1986, Astrophys. J. 301, 339 CrossRefGoogle Scholar