Modelling of the Magnetic Field of Solar Prominences

Anzer, U.

doi:10.1007/978-3-642-72640-8_6

U. Anzer²

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Abstract

Measurements of magnetic fields in quiescent prominences have a long tradition. Rust (1967) and Harvey (1969) made extensive studies of strengths and distributions of fields in prominences. Since they used the longitudinal Zeeman effect they could only obtain the line of sight component of the magnetic field B_ll. They found typical field strengths of about 20 Gauss in quiescent prominences. They did not say anything about the direction of the field with respect to the long axis of these prominences. Based on the large number of observational data Anzer and Tandberg-Hanssen (1971) took a statistical approach to find a general trend for this field orientation. They found that in general the field crosses the prominence at a small angle of the order of 15°.

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References

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Institut für Astrophysik, Max-Planck-Institut für Physik und Astrophysik, Karl-Schwarzschild-Str. 1, D-8046, Garching, Fed. Rep. of Germany
U. Anzer

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U. Anzer
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Institut für Astrophysik, Max-Planck-Institut für Physik und Astrophysik, Karl-Schwarzschild-Str. 1, D-8046, Garching, Fed. Rep. of Germany
Wolfgang Hillebrandt , Emmi Meyer-Hofmeister & Hans-Christoph Thomas , &

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Anzer, U. (1987). Modelling of the Magnetic Field of Solar Prominences. In: Hillebrandt, W., Meyer-Hofmeister, E., Thomas, HC. (eds) Physical Processes in Comets, Stars and Active Galaxies. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-642-72640-8_6

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DOI: https://doi.org/10.1007/978-3-642-72640-8_6
Publisher Name: Springer, Berlin, Heidelberg
Print ISBN: 978-3-642-72642-2
Online ISBN: 978-3-642-72640-8
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