Probing the physics of the solar atmosphere with the Multi-slit Solar Explorer (MUSE): I. Coronal Heating. (arXiv:2106.15584v1 [astro-ph.SR])

Probing the physics of the solar atmosphere with the Multi-slit Solar Explorer (MUSE): I. Coronal Heating. (arXiv:2106.15584v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Pontieu_B/0/1/0/all/0/1">Bart De Pontieu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Testa_P/0/1/0/all/0/1">Paola Testa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Martinez_Sykora_J/0/1/0/all/0/1">Juan Martinez-Sykora</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Antolin_P/0/1/0/all/0/1">Patrick Antolin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Karampelas_K/0/1/0/all/0/1">Konstantinos Karampelas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hansteen_V/0/1/0/all/0/1">Viggo Hansteen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rempel_M/0/1/0/all/0/1">Matthias Rempel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cheung_M/0/1/0/all/0/1">Mark C. M. Cheung</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Reale_F/0/1/0/all/0/1">Fabio Reale</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Danilovic_S/0/1/0/all/0/1">Sanja Danilovic</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pagano_P/0/1/0/all/0/1">Paolo Pagano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Polito_V/0/1/0/all/0/1">Vanessa Polito</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moortel_I/0/1/0/all/0/1">Ineke De Moortel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nobrega_Siverio_D/0/1/0/all/0/1">Daniel Nobrega-Siverio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Doorsselaere_T/0/1/0/all/0/1">Tom Van Doorsselaere</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Petralia_A/0/1/0/all/0/1">Antonino Petralia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Asgari_Targhi_M/0/1/0/all/0/1">Mahboubeh Asgari-Targhi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Boerner_P/0/1/0/all/0/1">Paul Boerner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carlsson_M/0/1/0/all/0/1">Mats Carlsson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chintzoglou_G/0/1/0/all/0/1">Georgios Chintzoglou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Daw_A/0/1/0/all/0/1">Adrian Daw</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+DeLuca_E/0/1/0/all/0/1">Ed DeLuca</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Golub_L/0/1/0/all/0/1">Leon Golub</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Matsumoto_T/0/1/0/all/0/1">Takuma Matsumoto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ugarte_Urra_I/0/1/0/all/0/1">Ignacio Ugarte-Urra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McIntosh_S/0/1/0/all/0/1">Scott McIntosh</a>, the <a href="http://arxiv.org/find/astro-ph/1/au:+team_MUSE/0/1/0/all/0/1">MUSE team</a>

The Multi-slit Solar Explorer (MUSE) is a proposed NASA MIDEX mission,
currently in Phase A, composed of a multi-slit EUV spectrograph (in three
narrow spectral bands centered around 171A, 284A, and 108A) and an EUV context
imager (in two narrow passbands around 195A and 304A). MUSE will provide
unprecedented spectral and imaging diagnostics of the solar corona at high
spatial (<0.5 arcsec), and temporal resolution (down to ~0.5s) thanks to its
innovative multi-slit design. By obtaining spectra in 4 bright EUV lines (Fe IX
171A , Fe XV 284A, Fe XIX-Fe XXI 108A) covering a wide range of transition
region and coronal temperatures along 37 slits simultaneously, MUSE will for
the first time be able to “freeze” (at a cadence as short as 10 seconds) with a
spectroscopic raster the evolution of the dynamic coronal plasma over a wide
range of scales: from the spatial scales on which energy is released (~0.5
arcsec) to the large-scale often active-region size (170 arcsec x 170 arcsec)
atmospheric response. We use advanced numerical modeling to showcase how MUSE
will constrain the properties of the solar atmosphere on the spatio-temporal
scales (~0.5 arcsec, ~20 seconds) and large field-of-view on which various
state-of-the-art models of the physical processes that drive coronal heating,
solar flares and coronal mass ejections (CMEs) make distinguishing and testable
predictions. We describe how the synergy between MUSE, the single-slit,
high-resolution Solar-C EUVST spectrograph, and ground-based observatories
(DKIST and others) can address how the solar atmosphere is energized, and the
critical role MUSE plays because of the multi-scale nature of the physical
processes involved. In this first paper, we focus on how comparisons between
MUSE observations and theoretical models will significantly further our
understanding of coronal heating mechanisms.

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