HOP 0232

abstract of observational proposal

X-ray jets are most commonly observed in coronal hole regions (Sako et al. 2013), and most observations of them have been in the polar coronal holes (CHs). To understand their structure better, we will observe them in an on-disk CH. This will allow us to investigate their magnetic environment more easily than possible with the polar CH case.

In addition to observing their structure and thermal characteristics with XRT, we will examine their spectral properties with EIS, and we will look for possible Ca signatures and examine FG magnetic data with SOT. This will be a Target of Opportunity (ToO) HOP, with the proposers notifying the Hinode operators when a suitable situation occurs to run the HOP (including a good on-disk coronal hole target).

X-ray jets somewhat preferentially (by about a factor of three) occur near the polar CH boundary compared to the CH center (Sako et al. 2013), and therefore we will aim to have the boundary at the edge of the XRT FOV. It is acceptable for SOT's FOV to include only the CH central region, if the CH is larger than the SOT FOV.

request to SOT

- Ca at reasonably-high cadence (20 sec). FG magnetograms once every ~2 - ~3 minutes. No SP observations are needed. FOV 128 x ~240. Double binned.

The estimated telemetry usage is <~240 Mbit/6 hr (= 480 Mbit/12 hour).

request to XRT

Al-poly filter with cadence of 30 sec, together with Al-mesh at the same cadence or at a lower cadence if necessary for telemetry (~1 min). Exposure time should be as long as possible that is safe for the instrument; probably 4 sec.

FOV: 384 x 384 pix, =400'' X 400''

Compression: Q90

Please use the HOP 81 XOB for these observations.

The estimated telemetry usage is <~47 Mbit/6 hours (=94 Mbit/12 hours).

request to EIS

The EIS study is intended to cover a large area in a reasonable time while retaining a number of good diagnostics. Only snapshots of jets will be
possible due to the cadence, but previous studies suggest a number of jets should be observed over a period of several hours. The study name is

"ISSI_jet_1," and the parameters are:

Duration: 1hr 2min
Slit: 2"
Step size: 3"
Raster size: 180"x336"
Exposure time: 56s
Data volume: 27.8 MBit
Data rate: 7.4 kBit/s
Compression: JPEG92

The study should be repeated to fill the available time slot. For EIS purposes, the time slot is recommended to be at least 12 hours. The data volume over 12 hours would be 323 MBit.

remarks

Target: On-disk coronal hole, within ~2.5 days of disk center. This is a To HOP, and the proposing team will notify the Hinode team when an appropriate target appears.

Pointing: At least one of the CH boundaries should be within the XRT FOV, but that boundary should be near the edge of the XRT FOV. It is acceptable for SOT's FOV to be totally inside the CH. But if the CH is not too large, please include a CH boundary in the SOT FOV, as long as XRT can still see the entire CH.

Time and Duration: The default request twelve hours per run if planning considerations allow, but no shorter than six hours. Please include the SAA-free time period if possible. Interruptions for standard synoptics is acceptable. Run repeatedly on successive days if solar conditions permit.

Other instruments: Other instruments, e.g., ground based, may participate in some runs of the HOP, but the default mode is Hinode alone. The HOP proposers
will notify the Hinode planners if other instrument observing times need to be considered in preparing the Hinode plan.