HOP 0053

HOP No.

HOP title

HOP 0053

CORE: SOT continuous magnetic field observations for investigating mechanisms responsible for XBPs and QS dynamics

plan term

2007/12/10-2007/12/16
2007/12/17-2007/12/23
2007/12/24-2007/12/30
2008/01/01-2008/01/03
2008/01/21-2008/01/27
2008/02/01-2008/02/28

abstract of observational proposal

Previous magnetic-field observations (/w 1-2 arcsec spatial resolution,
longitudinal only) shows that magnetic cancellation is involved in many XBPs
and magnetic emergence in a limited number of XBPs (e.g., Harvey et al.)
Priest and Parnell (1994) proposed a magnetic canceling model for explaining
the overall evolution of XBPs. However, this model has not yet been confirmed
with observations. SOT has not yet performed magnetic-field observations
suitable for investigating mechanisms responsible for XBPs (see Kotoku et
al. 2007 PASJ). The biggest problem in the observations made so far with Hinode
is that continuous SOT observations are available only in a few - several hours,
which is much shorter than the lifetime of XBPs (8 hrs for small typical XBPs,
48hrs for bigger XBPs) and time-scale of small-scale magnetic field evolution
(Schrijver et al. 1998). We are lack of observations with continuous a-few
days tracking of a quiet region with Hinode SOT coodinated with XRT and EIS.

request to SOT

SOT magnetic-field observation is the core observation. Because of telemetry
bandwidth limit, the following order is given to the priority. Run
the continuous sequence (with medium data flow rate) for most of
the observing period,
1) Highest priority - NFI Stokes I/V NaID (with dopplergram)
FOV 164”x164” (1K x 1K, 2x2), 1-2 min cadence
2) Second priority - BFI G-band and CaIIH images
FOV equivalent to NFI (1.5K x 1K, 2x2), 1-2 min cadence
3) Second priority - SP fast map FOV 164”x164”, 1hr or less cadence,
depending on the DR telemetry capacity
The template program was run in 10/10 18:45 - 10/11 8:00 & 10/11 14:00-10/12
3:00UT. The sequence can be adjusted, depending on the allowable telemetry.

request to XRT

* A test of HOP53 (XBP observation) performed from 11/30 18:22:30 to 11/30 18:50:24. The following XOBs can be used for this purpose.

* XOB #1473: QS thermal -FOV384x256 -AEC1 and AEC3 (single-high)
* XOB #1474: QS thermal -FOV384x256 -AEC1 and AEC3 (pair-med)
Both for a test of HOP53.

remarks

This Hinode coordinated observation needs to track one target region (quiet Sun)
near the disk center for two or three-successive days. It is acceptable to
interrupt this continuous observation by having XRT synoptic observations
every 6 hours. This proposal is driven by the Hinode core team members, since
we cannot perform such continuous observations as a core program with the
current situation with many incoming HOP proposals.

We prefer to this opportunities at multiple times in December - January frame
for sampling XBPs as much as possible for statistical studies. One possible
opportunity would be in January 1 - January 3 because of Hinode operation
holiday period (although need to reduce the telemetry rate), but it would be
better to have another (at least one or two) opportunities in December and
January.