Title: JOP176 SHORT-TIMESCALE CORONAL HOLE EVOLUTION
Author: Barbara Bromage (bjibromage@uclan.ac.uk)
Received: 25 May 2004
Ideal conditions:
large, low-latitude coronal hole crossing the meridian.
Compromise conditions:
coronal hole boundary at lowest latitude available and as near to
the meridian as possible.
Observe:
for 3-5 days, twice per day, CDS study UCLAN_N4 (4'x4') run
three times consecutively on a section of the boundary,
allowing for rotation; the eastern boundary is preferred
initially.
Time taken: 3-5 x 2 x 3 = 18-30 hours (approx.)
Run UCLAN_N2 (3 repeats) once during this period, ideally
near the meridian, centred on the same boundary region.
Time taken: 4hrs (approx.)
EIT as well as synoptic observations, take EIT304 images about
once per hour, to include the region of the CDS observations,
not necessarily full-disc.
MDI synoptic 96-minute full disc magnetograms;
try to coordinate CDS obs with these (i.e. maximise the number
of simultaneous observations). If MDI has High Rate telemetry,
then produce full disc mags and dopplergrams at 1-minute
cadence if possible.
SUMER (if available) look for flows in the boundary region
using transition region and low coronal lines; maybe network
observations too?
AIMS:
Observe the network and boundary of a coronal hole to see what
the relationship is over time.
Measure quasi-instantaneous rotation rate of the coronal hole
and compare this with the overall rotation rate over one or
more rotations.
Measure the temperature and density in the boundary region and
look for flows in relation to changes in the boundary.
Total observing time (approx):
Over 3 days - 22 hours.
5 days - 34 hours.