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Horizontal Expansion of Eruptive Prominences

Published online by Cambridge University Press:  12 April 2016

Bogdan Rompolt
Bogdan Rompolt*
Affiliation:
Astronomical Institute of Wrocław University, 51-622 Wroclaw, ul. Kopernika 11, Poland

Extract

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It is well known that quiescent prominences (QPs) as well as active region prominences (ARPs) occasionally undergo eruptions. The process of eruption of these prominences is caused by eruption of a huge magnetic system (HMS) associated with the prominence channel and the prominence itself (Rompolt 1984). Material of these prominences is frozen-into only a part of such a magnetic system – before as well as during the eruption. When an HMS erupts it simply lifts with it the frozen-in prominence material.

Usually during the eruption a large part of the prominence material is lifted high into the corona and/or into interplanetary space. Nevertheless, on some occasions during the eruption a significant part of the original prominence material flows down to the chromosphere (Rompolt 1990).

Type
Birth and Death of Filaments
Information
International Astronomical Union Colloquium , Volume 167: New Perspectives on Solar Prominences , 1998 , pp. 330 - 333
Copyright
Copyright © Astronomical Society of the Pacific 1998

References

Rompolt, B. 1984, Adv. Space Res., 4, No. 4, 357 CrossRefGoogle Scholar
Rompolt, B. 1990, Hvar Obs. Bull., 14, 37 Google Scholar
Rudawy, P., Rompolt, B., Kotrč, P., Heinzel, P. and Knižek, M. 1994, in Solar Magnetic Fields, (eds.) Schlüsser, M. and Schmidt, W., Cambridge University Press, p. 372 Google Scholar