Tomography and the distribution of streamers in the extended solar corona: some implications for large-scale MHD models

Details Tomography and the distribution of streamers in the extended solar corona: some implications for large-scale MHD models Tomography and the distribution of streamers in the extended solar corona: some implications for large-scale MHD models

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh31a1790m&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SH31A-1790

Astronomy and Astrophysics

Astrophysics

[7509] Solar Physics, Astrophysics, And Astronomy / Corona, [7524] Solar Physics, Astrophysics, And Astronomy / Magnetic Fields, [7536] Solar Physics, Astrophysics, And Astronomy / Solar Activity Cycle

Scientific paper

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.

Affiliated with

Also associated with

No associations

Rating

Tomography and the distribution of streamers in the extended solar corona: some implications for large-scale MHD models does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Tomography and the distribution of streamers in the extended solar corona: some implications for large-scale MHD models, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Tomography and the distribution of streamers in the extended solar corona: some implications for large-scale MHD models will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1509031