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| Titel |
The link between CMEs, filaments and filament channels |
| VerfasserIn |
S. F. Martin, O. Panasenco, O. Engvold, Y. Lin |
| Medientyp |
Artikel
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| Sprache |
Englisch
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| ISSN |
0992-7689
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| Digitales Dokument |
URL |
| Erschienen |
In: Annales Geophysicae ; 26, no. 10 ; Nr. 26, no. 10 (2008-10-15), S.3061-3066 |
| Datensatznummer |
250016253
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| Publikation (Nr.) |
 copernicus.org/angeo-26-3061-2008.pdf |
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| Zusammenfassung |
| We present a broad concept for the build-up to eruptive solar events which
needs to be tested in future observational and theoretical research. In this
concept an eruptive solar event consists of a coronal mass ejection, a
filament eruption, a cavity around the filament, and a flare. In our
picture, the initial energy source must be external to this eruptive system
but also feed into it. Among all eruptive events the common denominator is a
filament channel with canceling magnetic fields along a primary polarity
reversal boundary. We find that magnetic reconnection at or close to the
photosphere is the only interpretation of canceling fields to date that is
consistent with observations of filament channels. This reconnection serves
to transfer magnetic flux from the photosphere into the chromosphere and
corona along polarity reversal boundaries and concurrently initiates the
building of a filament channel. Magnetic flux, in excess of that needed to
sustain the filament channel, goes into building a filament magnetic field
that is always aligned with the polarity reversal boundary and the channel
magnetic field. The filament magnetic field remains separated from
overarching coronal magnetic fields by the magnetic field of the cavity. The
magnetic flux being transported upward from the photosphere/chromosphere
carries streams of plasma into the corona along the filament magnetic field.
However, the flowing and counterstreaming filament mass also slowly drains
out of the field and thereby leaves behind new strands of cavity magnetic
field with little or no associated mass. When the build-up of magnetic
pressure in the filament and cavity magnetic fields exceeds that of the
overlying coronal loops, the coronal loops, the filament and the cavity
together begin an observable slow rise which can last a few hours to many
days before rapid onset and ejection with a solar flare. We suggest that
this process can be accelerated by any number of external triggering
mechanisms which serve as catalysts to cause the impending eruption to
happen earlier than it otherwise would occur. |
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