TY - CONF
T1 - Hot Prominence Cavities
AU - Habbal, Shadia Rifai
AU - Druckmuller, M.
AU - Morgan, H.
AU - Scholl, I.
AU - Rusin, V.
AU - Daw, A.
AU - Johnson, J.
AU - Arndt, M.
PY - 2010/5/1
Y1 - 2010/5/1
N2 - Multiwavelength observations of the solar corona made during the total
solar eclipses of 2006 March 29 and 2008 August 1, are used to study the
thermodynamic properties of prominence cavities. Historically, cavities
have been associated with the base of streamers where the white light
intensity is reduced compared to their surroundings. The exceptional
high spatial resolution close to 1 arcsec in the white light eclipse
images, show that they consist of arch-like envelopes, extending from
0.1 to 0.3 solar radii above prominences. They are invariably bright in
coronal emission lines, with their brightness varying with temperature.
For most of the cases observed, the cavities are dominated by emission
from the hotter, 2 MK Fe XIII 1074.7 and Fe XIV 530.3 nm lines, although
examples of cavities which were bright in the cooler 1 MK Fe X 637.4 and
Fe XI 789.2 nm lines, and dim in the hotter lines, were also found.
These observations resolve the long-standing ambiguity associated with
the temperature of cavities.
AB - Multiwavelength observations of the solar corona made during the total
solar eclipses of 2006 March 29 and 2008 August 1, are used to study the
thermodynamic properties of prominence cavities. Historically, cavities
have been associated with the base of streamers where the white light
intensity is reduced compared to their surroundings. The exceptional
high spatial resolution close to 1 arcsec in the white light eclipse
images, show that they consist of arch-like envelopes, extending from
0.1 to 0.3 solar radii above prominences. They are invariably bright in
coronal emission lines, with their brightness varying with temperature.
For most of the cases observed, the cavities are dominated by emission
from the hotter, 2 MK Fe XIII 1074.7 and Fe XIV 530.3 nm lines, although
examples of cavities which were bright in the cooler 1 MK Fe X 637.4 and
Fe XI 789.2 nm lines, and dim in the hotter lines, were also found.
These observations resolve the long-standing ambiguity associated with
the temperature of cavities.
UR - http://hdl.handle.net/2160/10566
M3 - Paper
ER -