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Prominence Oscillations and the Influence of the Distant Photosphere

Published online by Cambridge University Press:  12 April 2016

N.A.J. Schutgens ,
M. Kuperus  and
G.H.J. van den Oord
N.A.J. Schutgens
Affiliation:
Astronomical Institute Utrecht, Utrecht University, the Netherlands
M. Kuperus
Affiliation:
Astronomical Institute Utrecht, Utrecht University, the Netherlands
G.H.J. van den Oord
Affiliation:
Astronomical Institute Utrecht, Utrecht University, the Netherlands

Abstract

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We model vertical prominence dynamics, describing the evolution of the magnetic field in a self-consistent way. Since the photosphere imposes a boundary condition on the field (flux conservation), the Alfvén crossing time τ 0/2 between prominence and photosphere has to be taken into account. Using an electrodynamical description of the prominence we are able to compare two basic prominence models: Normal Polarity (NP) and Inverse Polarity (IP).

The results indicate that for IP prominences, the stability properties are sensitive to ωτ 0 (ω: oscillation frequency of prominence). For ωτ 0 ≳ 1 instability results. Forced oscillations of five minutes are efficiently excited in IP prominences that meet certain criteria only. NP prominences on the other hand, are insensitive to the Alfvén crossing time. Forced oscillations of five minutes are difficult to excite in NP prominences.

Type
Filaments and Their Environment
Information
International Astronomical Union Colloquium , Volume 167: New Perspectives on Solar Prominences , 1998 , pp. 147 - 150
Copyright
Copyright © Astronomical Society of the Pacific 1998

References

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