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The 2007 PROM Workshop will be held at
University of California Berkeley Campus on
Oct 29-30. The local contact is Brian Welsch.
The PROM collaborator contact is Sara Martin at
HelioResearch.
PROM Workshops are for detailed discussions
among participants on their research on the
topics of filaments and prominences and the
environment of these structures. As long as
the Workshops remain small, every participant
has up to 30 minutes to present their research.
Presentations are informal and discussion
usually occurs during the talks as well as at the
end of each talk. Both theoretical and
observational talks are encouraged.
The talks may include work in progress and
tend to focus on current basic issues that need
to be addressed to better understand the nature
of solar prominences, how they form, and how
they evolve. Equally important is new material
on filament/prominence environment: the
filament channel in the photosphere and
chromosphere as well as cavity and
surrounding coronal magnetic fields. Other
issues are the differences and similarities
between active region and quiescent filaments,
the origin of their chirality (observed forms that
indicate their sign of helicity), and their
relationship to coronal structures known as
sigmoids. More emphasis has previously been
placed on understanding the basic structure,
plasma motins and magnetic fields in both
filaments and filament channels in their
non-eruptive state.
However, recent data and advances now make
it more relevant to include how and why
prominences erupt along with coronal mass
ejections.
University of California Berkeley Campus on
Oct 29-30. The local contact is Brian Welsch.
The PROM collaborator contact is Sara Martin at
HelioResearch.
PROM Workshops are for detailed discussions
among participants on their research on the
topics of filaments and prominences and the
environment of these structures. As long as
the Workshops remain small, every participant
has up to 30 minutes to present their research.
Presentations are informal and discussion
usually occurs during the talks as well as at the
end of each talk. Both theoretical and
observational talks are encouraged.
The talks may include work in progress and
tend to focus on current basic issues that need
to be addressed to better understand the nature
of solar prominences, how they form, and how
they evolve. Equally important is new material
on filament/prominence environment: the
filament channel in the photosphere and
chromosphere as well as cavity and
surrounding coronal magnetic fields. Other
issues are the differences and similarities
between active region and quiescent filaments,
the origin of their chirality (observed forms that
indicate their sign of helicity), and their
relationship to coronal structures known as
sigmoids. More emphasis has previously been
placed on understanding the basic structure,
plasma motins and magnetic fields in both
filaments and filament channels in their
non-eruptive state.
However, recent data and advances now make
it more relevant to include how and why
prominences erupt along with coronal mass
ejections.
These H alpha images emphasize the three major structures of filaments: the spine, barbs,
and legs at the extreme ends. The spine is very narrow and runs the length of the long axis of
filaments. The spine is clearly identified in the two prominences at the east and west limbs of
the Sun in the two upper left frames. Extending from the spine to the chromosphere are the
barbs. The independence of the barbs on each side of the filament is illustrated in the filament
in the lower left on 2003 Aug 28. Various shapes of barbs are illustrated in the adjacent image
from 2004 Aug 10 which, due to perspective, show barbs on only one side of the filament. The
rooting of the ends of filaments in the chromosphere are clearest during the eruption of a
filament as illustrated in the image on 2004 Apr 30 on the right side. In this image, the
apparent middle leg is a barb in the process of detaching from the spine. The detachment is
taking place where the thin threads of the barb meet a bright section of the base of the spine
of the filament. Mass below the point falling down and mass above this point is moving
upward.
and legs at the extreme ends. The spine is very narrow and runs the length of the long axis of
filaments. The spine is clearly identified in the two prominences at the east and west limbs of
the Sun in the two upper left frames. Extending from the spine to the chromosphere are the
barbs. The independence of the barbs on each side of the filament is illustrated in the filament
in the lower left on 2003 Aug 28. Various shapes of barbs are illustrated in the adjacent image
from 2004 Aug 10 which, due to perspective, show barbs on only one side of the filament. The
rooting of the ends of filaments in the chromosphere are clearest during the eruption of a
filament as illustrated in the image on 2004 Apr 30 on the right side. In this image, the
apparent middle leg is a barb in the process of detaching from the spine. The detachment is
taking place where the thin threads of the barb meet a bright section of the base of the spine
of the filament. Mass below the point falling down and mass above this point is moving
upward.
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