Cheung, Mark C. M., Martínez-Sykora, Juan, Testa, Paola, De Pontieu, Bart, Chintzoglou, Georgios, Rempel, Matthias, Polito, Vanessa, Kerr, Graham S., Reeves, Katharine K., Fletcher, Lyndsay, Jin, Meng, Nóbrega-Siverio, Daniel, Danilovic, Sanja, Antolin, Patrick, Allred, Joel, Hansteen, Viggo, Ugarte-Urra, Ignacio, DeLuca, Edward, Longcope, Dana, Takasao, Shinsuke, DeRosa, Marc L., Boerner, Paul, Jaeggli, Sarah, Nitta, Nariaki V., Daw, Adrian, Carlsson, Mats, Golub, Leon and the MUSE team, (2022) Probing the Physics of the Solar Atmosphere with the Multi-slit Solar Explorer (MUSE). II. Flares and Eruptions. The Astrophysical Journal, 926 (1). p. 53. ISSN 0004-637X
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Abstract
Current state-of-the-art spectrographs cannot resolve the fundamental spatial (subarcseconds) and temporal (less than a few tens of seconds) scales of the coronal dynamics of solar flares and eruptive phenomena. The highest-resolution coronal data to date are based on imaging, which is blind to many of the processes that drive coronal energetics and dynamics. As shown by the Interface Region Imaging Spectrograph for the low solar atmosphere, we need high-resolution spectroscopic measurements with simultaneous imaging to understand the dominant processes. In this paper: (1) we introduce the Multi-slit Solar Explorer (MUSE), a spaceborne observatory to fill this observational gap by providing high-cadence (<20 s), subarcsecond-resolution spectroscopic rasters over an active region size of the solar transition region and corona; (2) using advanced numerical models, we demonstrate the unique diagnostic capabilities of MUSE for exploring solar coronal dynamics and for constraining and discriminating models of solar flares and eruptions; (3) we discuss the key contributions MUSE would make in addressing the science objectives of the Next Generation Solar Physics Mission (NGSPM), and how MUSE, the high-throughput Extreme Ultraviolet Solar Telescope, and the Daniel K Inouye Solar Telescope (and other ground-based observatories) can operate as a distributed implementation of the NGSPM. This is a companion paper to De Pontieu et al., which focuses on investigating coronal heating with MUSE.
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| Additional Information: | Funding information: We gratefully acknowledge support by NASA contract 80GSFC21C0011 (MUSE Phase A). Some of this work was also supported by NASA contract NNG09FA40C (IRIS) and NASA grants 19-HTMS19_2-0025, 80NSSC18K1285, 80NSSC21K0737, and 80NSSC19K0855. D.N.S. acknowledges funding from the Synergy grant No. 810218 (ERC-2018-SyG) of the European Research Council and the project PGC2018- 095832-B-I00 of the Spanish Ministry of Science, Innovation, and Universities. P.A. acknowledges funding from the STFC Ernest Rutherford Fellowship (No. ST/R004285/2). V.P. acknowledges support from NASA’s HGI grant# 80NSSC20K0716. L.F. acknowledges support from STFC Consolidated Grant ST/T000422/1. G.C., M.R. and MCMC acknowledge support from NASA grant 80NSSC19K0855 “Investigating the Physical Processes Leading to Major Solar Activity.” M.C.M.C. acknowledges support from NASA’s SDO/AIA contract (NNG04EA00C) to LMSAL. AIA is an instrument on board SDO, a mission for NASA’s Living with a Star program. G.S.K. acknowledges support from NASA’s Early Career Investigator Program (Grant# 80NSSC21K0460) and Heliophysics Supporting Research program (Grant# 80NSSC19K0859). The simulations have been run on clusters from the Notur project, and the Pleiades cluster through the computing project s1061, s8305, and s2169 from the High-End Computing (HEC) division of NASA. This material is based upon work supported by the National Center for Atmospheric Research, which is a major facility sponsored by the National Science Foundation under Cooperative Agreement No. 1852977. We would like to acknowledge high-performance computing support from Cheyenne (doi:10.5065/D6RX99HX) provided by NCAR’s Computational and Information Systems Laboratory, sponsored by the National Science Foundation. S.D. is supported by a grant from the Swedish Civil Contingencies Agency (MSB) and the Knut and Alice Wallenberg foundation (2016.0019). Simulation MURaM_emergence was performed on resources provided by the Swedish National Infrastructure for Computing (SNIC) and the European Unionʼs Horizon 2020 research and innovation program under grant agreement No. 824135 (SOLARNET). The synthesis and analysis of the various numerical models have been performed on the Google Cloud Platform, allowing sharing the synthetic data and models, developing common tools, and access to instances with various specifications and Graphics Processing Units (GPUs). This project has been supported by a grant (project lunar-campaign29341) by Google Could to the University of Oslo. |
| Uncontrolled Keywords: | Active solar corona, Solar coronal mass ejections, Solar coronal waves, Solar flares, Extreme ultraviolet astronomy, Solar extreme ultraviolet emission, Magnetohydrodynamics; Radiative magnetohydrodynamics, Astrophysical fluid dynamics, Solar instruments, Astronomical instrumentation |
| Subjects: | F300 Physics F500 Astronomy |
| Department: | Faculties > Engineering and Environment > Mathematics, Physics and Electrical Engineering |
| Depositing User: | John Coen |
| Date Deposited: | 15 Feb 2022 09:10 |
| Last Modified: | 15 Feb 2022 09:15 |
| URI: | http://nrl.northumbria.ac.uk/id/eprint/48462 |
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