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Proposal ID Aschwanden_25

Date of Proposal
96/08/19

firstname
Markus

lastname
Aschwanden

institute
University of Maryland

address
University of Maryland
Astronomy Dept
College Park, MD 20742, USA

email
markus@astro.umd.edu

phone
(301) 405-1525

fax
(301) 314-9067

proposal
During a Mini-Campaign on 1996 May 23, 24, and 26 we observed
with the VLA, OVRO, Yohkoh, SOHO, and KPNO the North coronal
hole, its boundary, and the West limb. The Sun was very quiet
during these 3 days, there was no active region present on the
disk. From the radio images taken at many different wavelengths,
the SXT images, and EUV images we plan to derive quantiative
coronal models of the electron density, temperature, differential
emission measure, filling factors from the deconvolution of
limb profiles in different wavelengths. For this purpose we like
to request EUV full-disk images taken during our observations,
in all 4 wavelengths covered by EIT, calibrated in physical
units (emission measure) if possible.

Furthe Collaborators: Tim Bastian (NRAO), Dale Gary (CALTECH),
Nariaki Nitta (Lockheed), Stu Jordan (SUMER), Paul Breeke (CDS)

inside_collab
Contact persons during observations (Barbara Thompson and Jeffrey
Newmark)

consortium
yes

topic
YOHKOH

topic

title
Temperature and Density Structure of Quiet Corona

update added on 1998/03/24 at 07:16:37
Update on March 24, 1998:
VLA maps from May 26, 1996, in X,C,L,P-band frequencies have been
reconstructed by Tim Bastian, where the solar limb is clearly
visible at all frequencies. M.Aschwanden did some preliminary
overlays with EIT images, but found some differences of order
10-50 arcseconds between the EUV and radio limb. In ongoing work
we attempt to establish the absolute coordinates of EIT images
in a more accurate way then provided in the EIT FITS headers to
get more reliable information on the relative offset of the limb
seen in EUV and radio.


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