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HINODE Operation Plan (HOP)

accepted on


 HOP No.

 HOP title

HOP 0039

SUMER campaign - Characterization of Fast and Slow Solar Wind Source Regions

plan term


@ @


 name : Miralles, Landi, Wilhelm @  e-mail : enrico.landi[at]nrl.navy.mil

contact person in HINODE team

 name : J. L. Culhane @  e-mail : jlc[at]mssl.ucl.ac.uk

 abstract of observational proposal
SCIENCE OBJECTIVE: We propose to study the sources of fast and slow
solar wind by investigating how the flux tubes change from a high-speed
to a low-speed region. We will select a polar hole with a clearly-defined streamer region nearby and study both regions and the boundary between the polar coronal hole and the surrounding quiet Sun region from the limb to UVCS heights. We aim to measure how the plasma physical properties change between the two wind regions, and with height, and how the flux tubes expand with
heliocentric distance. In particular, this campaign will study the evolution of the transition from fast to slow wind source regions as a function of time and heliocentric distance from the limb and will provide important experimental
constraints to theoretical models.

The present campaign will advance previous studies (e.g. Cranmer et al.
1999; Strachan et al. 2002; Landi et al. 2007) by examining the fast and slow
source regions and its transition as follow:

1 - centering the field of view on the boundary between the coronal hole
  and the quiet Sun
2 - using a much larger set of spectral lines
3 - extending the study to 2-4 R(sun) above the limb.

 request to SOT

 request to XRT

 request to EIS
EIS observations will consist of several repetitions of a single
sequence: a 25-step raster with the 2" slit that will observe the entire
EIS wavelength range downloading the central 400" of the EIS slit. The
exposure time is 150 s. and this study (which lasts about 1 hour and has
a data rate of ~53kbit/s) will be repeated at a few locations at
different heliocentric distances from the solar limb. We expect to run
it 7 times for a total of around 7 hours. The SUMER sequence will also
take around 7 hours to complete; the UVCS sequence will last longer.

 other participating instruments
UVCS will run this campaign from Nov 6 to 17, 2007. We request a joint
SUMER/EIS/UVCS observation coincidental with this time period.

SUMER and EIS will observe the same field of view at several positions
outside the solar limb up to the maximum distance allowed by their
pointing systems. UVCS will observe a set of temperature and outflow
diagnostic lines (including O VI and H I Lyman Alpha) at higher heights.

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