HOP 0187

abstract of observational proposal

The X-Ray Telescope (XRT) aboard the Hinode satellite has shown shown that polar coronal hole regions are very active with many X-ray jets and transient brightenings. Because the high-speed solar wind emanates from these regions, the relation between the solar wind and the coronal activity in the polar region is very important for understanding the high-speed solar wind. In order to understand this relationship, we propose a joint observation for tracking the materials ejected by X-ray jets from solar surface to interplanetary space.
Hinode and SDO observe from solar surface to inner corona, LASCO-C2/SOHO observes outer corona with deep exposure and high-time resolution, and the IPS system of STE Lab., Nagoya University observes interplanetary space. SECCHI/STEREO observes coronal activity from the either east or west of the Sun, and using the observations from these instruments we can investigate the 3D configuration of the transient structures in the polar solar regions. Based on the data obtained by the instruments, we will explore the following subjects:

・　How far does the influence of transient events in this region extend from the solar surface?

・　The kinetic/potential energies of the materials ejected by coronal activity and the importance of their energy in the solar wind.

・　The configuration of the magnetic field above the polar coronal hole based on the trajectory of the jets.

request to SOT

FG:
G-Band (BFI)
Field of View: 221" x 111", Pixel Summing: 2x2, Time resolution: 30 mins JPEG Quality: Q75
Remark: G-band images are used for co-alignment with XRT images.

Ca II H band (BFI)
Field of View: 221" x 111", Pixel Summing: 2x2, Time resolution: 2 mins JPEG Quality: Q75

Na I (NFI)
Field of View: 320" x 164", Pixel Summing: 2x2,Time resolution: 10 mins, Obs. mode: IVDG mode, JPEG Quality: Q75
Remark:
Time resolutions of the images depend on the condition of the downlink. Please contact M. Shimojo, if the CO needs to change the time resolutions.

SP: No requirement.

request to XRT

For X-ray observation:
Field of View: 395” x 395” (384 pix x 384 pix) #1
Center of FoV: the center of CCD.
X-ray Analysis filter: Al/mesh & Ti/Poly #2
Pixel Summing: none (1x1)
Exposure time: 16.34 sec & disable the AEC function. #3
JPEG Quality: Q95
Time resolution: less than 1 min for a filter pair.

Remark: Please take a dark image every 30 mins.

For G-band observation:
Field of View: 395” x 395” #1
Center of FoV: the center of CCD.
Filter: G-band
Pixel Summing: none (1x1)
Exposure time: 63 msec
JPEG Quality: Q98
Time resolution: 30 mins.

Remark: G-band images are used for co-alignment with SOT images.

#1: If we can use large data area, please change the FoV to 384 pix x 512 pix. In this case, the center of FoV is [1024, 896] in CCD-pixel coordinates.
#2: If we can use the filters of Filter Wheel 1, we request using the Al/poly and Thin-Be filters.
#3: Please contact Shimojo, if the CO needs to change the exposure time.

other participating instruments

-LASCO-C2/SOHO:
The LASCO team will provide the special LASCO-C2 observation with the high-time resolution and long exposure for the joint observation.

-SECCHI/STEREO
TBD

-SDO:
SDO will perform observations in its normal operating mode.

-STE-IPS:
The IPS system of STE Lab., Nagoya University observes the radio sources around the south region of the Sun and reveals the density fluctuations of heliosphere.

remarks

Target Region: Southern Polar Region (*1)
The Pointing Coordinate (Heliocentric coordinate) X: 0 arcsec, Y: -940 arcsec
Duration of the Observation: about 6 hours (*2)
Date and Time of the Observation: Middle of June (*3)

*1: In the northern polar region, the coronal hole has already become very small. Hence, we request an observation of the southern polar region in June.

*2: Continual observation is required, if possible.

*3: If the proposal is accepted, we will coordinate the actual date and times of the contact persons of the participating instruments.