The Solar High-Resolution X-ray imager (SHRX): A Concept for a Sounding Rocket Experiment
Abstract
The evolution and spatial distribution of small-scale, high-temperature plasma structures in the solar corona can be used to address multiple open science questions, including how the corona is dynamically heated, and how tremendous amounts of energy are released within seconds during eruptive events. Despite decades of imaging this plasma in X-rays, the spatial resolution of available grazing incidence mirrors has constrained our understanding of this important energy regime. High temperature plasma can be imaged in the extreme ultraviolet (EUV) using normal incidence telescopes, which can be more-readily fabricated to meet high resolution requirements. Multi-layers can be implemented to limit the narrow passband to select for EUV wavelengths containing high temperature emission lines. The EUV spectrum, however, contains cooler emission lines that inevitably contaminate high temperature channels. Here, we present a design concept for a high-resolution, (< 1 arcsecond) soft X-ray (SXR) imager to fly aboard a sounding rocket that will enable solar observations of small-scale structures containing plasma greater than 5 million degrees. The Solar High Resolution X-ray imager (SHRX) will observe a narrow SXR band centered at 1.03 keV (12 Angstroms) using cutting-edge multi-layer coatings and an improved glass substrate grazing incidence mirror developed at NASA Marshall Space Flight Center (MSFC). The optical design accommodates a CMOS detector developed by the Japan Aerospace Exploration Agency (JAXA), and previously flown aboard the FOXSI-3 sounding rocket. The detector consists of a 2k X 2k chip, 7 micron square pixel size, and rapid readout time enabling photon-counting capability. The science objective is to study small-scale, active region plasma flows associated with dynamic energy release. Within the constraints of a sounding rocket experiment, this will be accomplished via sub-arcsecond SXR observations of active region core plasma in a bandpass that overlaps with the temperature responses of Hinode/XRT and the SDO/AIA 94Å channel. The effective area curve of the mirror will be tuned via the mirror prescription and the multi-layer coating, which will shape the temperature response of the instrument. Here we present our science objectives and a technical overview of the instrument concept.
- Publication:
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AGU Fall Meeting Abstracts
- Pub Date:
- December 2019
- Bibcode:
- 2019AGUFMSH31C3318C
- Keywords:
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- 7534 Radio emissions;
- SOLAR PHYSICS;
- ASTROPHYSICS;
- AND ASTRONOMY;
- 7549 Ultraviolet emissions;
- SOLAR PHYSICS;
- ASTROPHYSICS;
- AND ASTRONOMY;
- 7554 X-rays;
- gamma rays;
- and neutrinos;
- SOLAR PHYSICS;
- ASTROPHYSICS;
- AND ASTRONOMY;
- 7594 Instruments and techniques;
- SOLAR PHYSICS;
- ASTROPHYSICS;
- AND ASTRONOMY