HOP list   Monthly Events

HINODE Operation Plan (HOP)

accepted on

22-feb-2018


 HOP No.

 HOP title

HOP 0349

XRT full-sun image campaign toward solar minimum

plan term

ToO
2018/06/11-2018/06/17
2018/08/07-2018/08/14
2018/08/29-2018/08/29
2018/08/31-2018/08/31
2018/09/05-2018/09/05
2018/09/09-2018/09/09
2018/09/16-2018/09/16
2018/09/19-2018/09/19
2018/09/21-2018/09/21
2018/09/24-2018/09/25
2018/09/28-2018/09/30
2018/10/03-2018/10/03
2018/10/05-2018/10/05
2018/10/07-2018/10/07
2018/10/10-2018/10/10
2018/10/12-2018/10/12
2018/10/14-2018/10/14
2018/10/17-2018/10/17
2018/10/19-2018/10/19
2018/10/21-2018/10/21
2018/10/24-2018/10/24
2018/10/27-2018/10/28
2018/10/31-2018/10/31
2018/11/02-2018/11/11
2018/11/15-2018/11/27
2018/12/07-2018/12/10
2018/12/12-2018/12/13
2018/12/16-2018/12/16
2018/12/18-2018/12/23
2018/12/27-2018/12/29
2019/01/08-2019/01/13
2019/01/17-2019/01/21
2019/01/23-2019/02/03
2019/02/06-2019/02/12
2019/02/14-2019/02/14
2019/02/17-2019/02/23
2019/02/17-2019/02/24
2019/03/01-2019/03/17
2019/03/21-2019/03/25
2019/03/27-2019/03/29
2019/04/03-2019/04/03
2019/04/06-2019/04/07
2019/04/20-2019/04/20
2019/04/24-2019/04/25
2019/04/27-2019/04/28
2019/04/30-2019/04/30
2019/05/01-2019/05/05
2019/05/09-2019/05/14

@ @

proposer

 name : Takeda @  e-mail : takeda[at]solar.physics.montana.edu

contact person in HINODE team

 name : DeLuca, Reeves @  e-mail : edeluca[at]cfa.harvard.edu, kreeves[at]cfa.harvard.edu

 abstract of observational proposal
Main Objective:
Full-Sun multi-filter observation by XRT

Scientific Justification:
This campaign requests to allocate a few hours of disk center pointing hopefully every day outside the period of other HOPs and core observations (e.g., AR tracking). The main purpose of this campaign is to increase the number of XRT's synoptic type images(fullsun images by multi-filters) per day. XRT synoptic images are used to derive soft X-ray solar irradiance by combining the filter-ratio analysis of the disk-integrated XRT signals with the calculation of energy flux (W/m^2) emitted from the model coronal plasma in a given wavelength range (e.g., 1-8A).

The soft X-ray irradiance obtained with Yohkoh/SXT (1991-2001) in the same method had an excellent correlation with the GOES/XRS 1-8A flux except the period around the solar minimum. Around the solar minimum, the solar flux went close or under the detection limit of GOES/XRS, but Yohkoh/SXT consistently yielded the irradiance values under 10^(-8)W/m^2. This shows the advantage of the filter-ratio irradiance over the GOES/XRS when the solar activity is approaching to the minimum (as of this writing, no information is yet delivered regarding the performance of the new XRS instrument on-board GOES-16 launched in late 2016). To perform the irradiance study with XRT filter-ratios, it is highly preferable to increase the number of data set to improve
the time resolution. Another purpose of this campaign is to watch the full-disk corona for catching eruptive events from unexpected places. While the ARs as a source of flares and CMEs are decreasing in both numbers and sizes in coming few years, eruptive events can also occur from quieter regions (e.g., a part of filament or old plage region). Since such events are often associated with the heated plasma that is efficiently detected in soft X-ray, full-disk image sequences obtained with XRT will provide unique data set to study eruptive events over other full-disk instruments using the light from cooler plasma.

 request to SOT
None

 request to XRT
Regular synoptic program (Al_mesh, Al_poly and thin_Be, 2x2 binning), every 2 hours with the CME watch program in between with Al_mesh, Al_poly and thin_Be, 4x4 binning, long and short exposure pairs every 1 to 5 minutes. Run this program at least 2 hours, but if telemetry permits, the longer hours are more preferable.

 request to EIS
None

 other participating instruments
None

 remarks
Target(s) of interest: Full disk solar corona

Additional Remarks:
From: Aki TAKEDA <takeda@mithra.physics.montana.edu>
Subject: [xrt_manager] a new plan for synoptics+HOP 349 run time.
Date: July 24, 2018 at 1:21:59 PM EDT
To: xrt_manager@head.cfa.harvard.edu
Cc: Aki TAKEDA <takeda@mithra.physics.montana.edu>

- start HOP349 at ~3UT daily until the morning synoptics,
then run a synoptics program as usual.
- keep the evening synoptics at ~18UT for 10-min.

---
Do not combine this program with the regular synoptics usually running at 6 and 18UT. One purpose of this program is to increase the opportunities of taking synoptic images. Preferable run time is therefore between the two synoptics (i.e., sometime between 8-16UT and/or 20-4UT).

Previous HOP information: No prior HOPs

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