TY - CONF
T1 - Tomography and the distribution of streamers in the extended solar corona: some implications for large-scale MHD models
AU - Morgan, H.
AU - Habbal, Shadia Rifai
PY - 2010/12/1
Y1 - 2010/12/1
N2 - cycle. Streamers are most often shaped as extended, often very narrow,
plasma sheets. At most times outside the height of solar maximum, there
are two separate stable large helmet streamer belts extending from
mid-latitudes (in both North and South). At solar minimum, the streamers
converge and join near the equator, giving the impression of a single
large helmet streamer. Outside of solar minimum, the two streamers do
not join, forming separate high-density sheets in the extended corona
(one in the North, another in the South). At solar maximum, streamers
rise radially from their source regions, whilst during the ascending and
descending activity phases, streamers are skewed towards the equator.
For most of the activity cycle, streamers share the same latitudinal
extent as filaments on the disk, showing that large-scale stable
streamers are closely linked to the same large-scale photospheric
magnetic configuration which give rise to large filaments. The polewards
footpoints of the streamers are often above crown polar filaments and
the equatorial footpoints are above filaments or active regions (or
above the photospheric neutral lines which underlie these structures).
The high-density structures arising from the equatorial active regions
either rise and form the equatorial footpoints of mid-latitude quiescent
streamers, or form unstable streamers at the equator, not connected to
the quiescent streamer structure at higher latitude (so there are often
three streamer sheets sharing the same extended longitudinal region).
Comparison between the tomography results and a potential field source
surface model shows that streamers are not necessarily associated with a
magnetic polarity reversal, but rather are regions containing field
lines arising from widely-separated sources at the Sun. We call these
convergence sheets (sometimes called 'pseudostreamers'). Large-scale
coronal MHD models could improve their agreement with observation by
incorporating the results of tomography.
AB - cycle. Streamers are most often shaped as extended, often very narrow,
plasma sheets. At most times outside the height of solar maximum, there
are two separate stable large helmet streamer belts extending from
mid-latitudes (in both North and South). At solar minimum, the streamers
converge and join near the equator, giving the impression of a single
large helmet streamer. Outside of solar minimum, the two streamers do
not join, forming separate high-density sheets in the extended corona
(one in the North, another in the South). At solar maximum, streamers
rise radially from their source regions, whilst during the ascending and
descending activity phases, streamers are skewed towards the equator.
For most of the activity cycle, streamers share the same latitudinal
extent as filaments on the disk, showing that large-scale stable
streamers are closely linked to the same large-scale photospheric
magnetic configuration which give rise to large filaments. The polewards
footpoints of the streamers are often above crown polar filaments and
the equatorial footpoints are above filaments or active regions (or
above the photospheric neutral lines which underlie these structures).
The high-density structures arising from the equatorial active regions
either rise and form the equatorial footpoints of mid-latitude quiescent
streamers, or form unstable streamers at the equator, not connected to
the quiescent streamer structure at higher latitude (so there are often
three streamer sheets sharing the same extended longitudinal region).
Comparison between the tomography results and a potential field source
surface model shows that streamers are not necessarily associated with a
magnetic polarity reversal, but rather are regions containing field
lines arising from widely-separated sources at the Sun. We call these
convergence sheets (sometimes called 'pseudostreamers'). Large-scale
coronal MHD models could improve their agreement with observation by
incorporating the results of tomography.
UR - http://hdl.handle.net/2160/10567
M3 - Paper
SP - 1790
ER -