HOP 0480

abstract of observational proposal

Main Objective: To perform coordinated observation with the HiC-FOXSI solar flare sounding rocket campaign

Scientific Justification: The solar flare sounding rocket campaign aims to observe a solar flare (> C5 class) near-simultaneously in multi-wavelengths (EUV through hard X-rays) using different high sensitivity instruments [HiC (EUV), FOXSI( soft X-rays & hard X-rays), SSAXI (soft X-rays), CoolAid(EUV)]. It aims to probe some of the fundamental questions of solar flares such as (a) understanding the mechanism of particle acceleration in solar flares, (b) studying the relationship between supra-arcade downflows and reconnection process, and (c) investigation of plasma heating mechanisms and determining the effects of energy input into the chromosphere. We propose to perform coordinated observations between Hinode EIS and the flare campaign instruments during the upcoming flight, in order to get an unprecedented coverage of plasma diagnostics (such as temperature, density) of the flaring region and take advantage of an invaluable opportunity for coordinated solar science. We propose EIS observations with the widest slot, sit and stare mode, and with the entire detector, to determine spectrally pure maps of the FOV. This provides a unique opportunity to cross-validate inversion of EIS spectroheliogram data in conjunction with observations from the sounding rocket observations, which will be helpful for several upcoming solar space missions.

Dates: Start date to End date : 5 April 2024 to 19 April 2024. We also request for a trial run in coordination with XRT observations in early March 2024.
Reason : Two-week window is assigned for the solar flare sounding rocket campaign. Date of launch will be fine-tuned based on solar activity.
Consecutive days are desired.

request to EIS

EIS study ID: 649
DHB_HiC_FOXSI_01

EIS will respond to the XRT flare trigger.
Set up hunter study Flare266_Hunter01 and enable the XRT flare trigger with response study #649 DHB_HiC_FOXSI_01.
Run each day during observing window 19:45 - 00:00 UT

-----
Observation of the entire EIS detector is desired, but not required. However, observation should cover the entire long wavelength channel detector and list of lines in the short wavelength channel outlined below. This requirement is important to perform high-fidelity inversion on the EIS spectroheliogram data. An EIS study fulfilling these requirements is currently being designed and verified. The basic outline is as follows.

This is a 266" (full CCD) slot Sit and Stare study designed to coordinate flare observations with the flare sounding rocket campaign.

TARGET : Flaring Active Region
SLIT : 266" slot
FOV : 266"x256"
EXPOSURE TIME : 25s
DELAY : - (TBD)
DURATION : - (TBD)
VOLUME : 3 Mbits per exposure (for full detector)
COMPRESSION : JPEG75

List of EIS lines required : Entire detector for long wavelength channel and the following line list for the short wavelength channel.

Required EIS line linst for SW channel
ION WAVELENGTH (ANG) ION WAVELENGTH (ANG)
FeX 174.531 FeX 177.24
FeXI 180.401 FeXI 182.167
FeX 184.537 FeVIII 185.213
FeVIII 186.598 FeXII 186.854
FeXII 186.887 FeXI 188.216
FeXI 188.299 FeIX 188.493
FeIX 189.935 FeX 190.037
FeXII 190.04 FeXII 192.394
FeXI 192.813 FeXII 193.509
FeVIII 194.661 FeXII 195.119
FeXIII 196.525 FeXII 196.64
FeIX 197.854 FeXIII 200.021
FeXIII 202.044 FeXI 202.705
FeXII 203.728 FeXIII 203.795
FeXIII 203.826 FeXIII 204.942
FeXIII 209.916 FeXIV 211.317
-----

remarks

Dates: Start date to End date : 5 April 2024 to 19 April 2024. We also request for a trial run in coordination with XRT observations in early March 2024.
Reason : Two-week window is assigned for the solar flare sounding rocket campaign. Date of launch will be fine-tuned based on solar activity.
Consecutive days are desired.

Time window: 19:45 - 00:00 UT

Target(s) of interest: active region

Previous HOPs: No prior HOP from PI

Additional remarks:
As this EIS request for full ccd would result in large data volume for long duration time window, like for the flare coordination, if possible we can run in flare trigger mode with He II images and then respond to the flare with the full CCD slot study.