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PROM WORKSHOP 2006
The 2006 PROM Workshop will be held at George Mason
University, Fairfax Campus in Fairfax, Virginia from October
30-31. The local contact is Arthur Poland. 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.
The 2006 PROM Workshop will be held at George Mason
University, Fairfax Campus in Fairfax, Virginia from October
30-31. The local contact is Arthur Poland. 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.
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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