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PROM WORKSHOP 2006
The 2006 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.org.
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 now more
relevant to include how and why prominences erupt along
with coronal mass ejections.
The 2006 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.org.
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 now more
relevant to include how and why prominences erupt along
with coronal mass ejections.
Active region filaments and surges amidst H alpha
chromospheric fine structure in the H alpha line;
recorded on 2005 Oct. 2004 at the Swediish Solar
Observatory by Yong Lin in the group of O. Engvold
from the Theoretical Institute for Astrophysics,
University of Oslo. The Swedish 1-m Solar Telescope
is operated on the island of La Palma by the Institute
for Solar Physics of the Royal Swedish Academy of
Sciences in the Spanish Observatorio del Roque de
los Muchachos of the Instituto de Astrofísica de
Canarias.
chromospheric fine structure in the H alpha line;
recorded on 2005 Oct. 2004 at the Swediish Solar
Observatory by Yong Lin in the group of O. Engvold
from the Theoretical Institute for Astrophysics,
University of Oslo. The Swedish 1-m Solar Telescope
is operated on the island of La Palma by the Institute
for Solar Physics of the Royal Swedish Academy of
Sciences in the Spanish Observatorio del Roque de
los Muchachos of the Instituto de Astrofísica de
Canarias.
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