HOP 0509

proposer

name :

Tamburri, Kowalski, Cauzzi, Kazachenko, Tritschler, French, Yadav, Reardon, Notsu

e-mail :

cole.tamburri[at]colorado.edu, adam.f.kowalski[at]colorado.edu, gcauzzi[at]nso.edu, maria.kazachenko[at]lasp.colorado.edu, ali[at]nso.edu, rfrench[at]lasp.colorado.edu, Rahul.Yadav[at]lasp.colorado.edu, kreardon[at]nso.edu, yuta.notsu[at]colorado.edu

abstract of observational proposal

Main Objective: We aim to co-ordinate flare observations with DKIST, IRIS, and Hinode in summer 2025.

Scientific Justification: As advances in the capabilities of solar observing have made the sizes of fundamental UV ribbon and WL/HXR kernel structures associated with solar flares progressively smaller (now on the order of 10-100km), the solar community has become more capable than ever of explaining the spatial distribution in physical mechanisms driving flare heating. Specifically, have yet to fully understand the processes driving differences in broadening of chromospheric lines such as members of the Balmer series, Ca II H and K, and the Mg II lines, all observed in emission during a solar flare.

Our DKIST experiment, which will be run in summer of 2025, seeks to understand chromospheric line broadening during a solar flare by observing the Ca II H, H-epsilon, and H-alpha, in addition to the Na I D1 line. The high-resolution capabilities of the DKIST mean that we will have the opportunity to study the spatially-dependent evolution of flare spectra at unprecedented resolution. We will compare our observations to modern RHD models (RADYN and RH) in order to constrain parameters relevant to electron beam heating, including potential spatial differences in the beam parameters driving an RHD simulation. As a result, it will be invaluable to have measurements of the X-ray emission from Hinode to provide context for our observations and modeling, as these data are signatures of the heating processes we are fundamentally interested in. We plan to include additional chromospheric lines (Mg II h&k) provided by IRIS and EIS/XRT on Hinode will provide further context for the flare region.

request to EIS

Run 'Flare266_Hunter01' study, switching to 'FlareRespAtlas10trm/652' study when a flare is triggered. Run to overlap with DKIST and IRIS (telemetry permitting).

FlareRespAtlas10trm/652 is a flare response with a nearly full CCD readout, the edges of the ccd have been cut out. This study provides a high cadence and large wavelength coverage for flare observations. As such, it enables the use of many lines not typically observed in flare responses.

other participating instruments

IRIS requests:
Co-ordinated observations already approved by IRIS team. Configuration listed below:

3665102935 | Medium dense 16-step raster 5x60 16s C II Mg II h/k Mg II w Deep | 19.92 | 27.24 | 0.93 | 1.2+/-0.1 | 19.9+/-0.0 | 10.0+/-0.1 | 0.0+/-0.0 | 9.9+/-0.1 | 9.9+/-0.1

Additional instrument coordination:
DKIST: H-alpha, H-epsilon/Ca II H, Na I D1 lines (ViSP); blue continuum filter (VBI); He I 10830, Fe I 1565 (DL-NIRSP)

ViSP slit details: intensity mode; slit width .1", 100 exposures, 10.71" FoV, anticipated map cadence of 13s

VBI details: blue channel only, 45"x45" FoV

DL-NIRSP: 4x20 mosaic, covering ~6"x35" FoV in ~12 min

remarks

Dates: To our knowledge, observations with the DKIST will occur between late May and early August. The target will be established once a Major Flare Watch is released. We are uncertain of our place on that list. We will know the target by 9 a.m. the day before observations are taken, and likely will know that our experiment will be run at least two days before hand.

Time window: Observing times of DKIST (daylight hours), no interruptions.

Target(s) of interest: Active region, predicted to be flare productive, in coordination with DKIST. We will inform DKIST, IRIS, and Hinode teams of the pointing of the telescope at 9AM pacific time, the day before observations.

Previous HOPs: None

Additional remarks:
This request is in the context of Cycle 3 PI-led DKIST/IRIS coordination testing