Abstract
Observations of Class I OH maser sources show a range of features which are predicted on the basis of Zeeman splitting in a source magnetic field. Magnetic field strengths of 2 to 7 mG are derived for eight OH maser sources. The fields in all the clouds are directed in the sense of galactic rotation. A model of W3 OH is proposed which incorporates the magnetic field data. It is shown that no large amount of magnetic flux or angular momentum has been lost since the condensation from the interstellar medium began.
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Davies, R.D. (1974). Magnetic Fields in OH Maser Clouds. In: Kerr, F.J., Simonson, S.C. (eds) Galactic Radio Astronomy. International Astronomical Union/ Union Astronomique Internationale, vol 60. Springer, Dordrecht. https://doi.org/10.1007/978-94-010-2263-7_33
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DOI: https://doi.org/10.1007/978-94-010-2263-7_33
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