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PROM WORKSHOP 2005
The 2005 PROM Workshop will be held at the High Altitude
Observatory (HAO) in Boulder, Colorado from October 27-29.
The local contact is Sarah Gibson. 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 2005 PROM Workshop will be held at the High Altitude
Observatory (HAO) in Boulder, Colorado from October 27-29.
The local contact is Sarah Gibson. 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 filament prominence and quiescent
filament taken at the Swediish Solar Observatory by
O. Engvold and colleagues 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.
filament taken at the Swediish Solar Observatory by
O. Engvold and colleagues 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.