Probing the Physics of the Solar Atmosphere with the Multi-slit Solar Explorer (MUSE). I. Coronal Heating
Probing the Physics of the Solar Atmosphere with the Multi-slit Solar Explorer (MUSE). I. Coronal Heating
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DOI：
10.3847/1538-4357/ac4222
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发表时间：
2021-06
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通讯作者：
B. De Pontieu;P. Testa;J. Martínez-Sykora;P. Antolin;K. Karampelas;V. Hansteen;M. Rempel;M. Cheung;F. Reale;S. Danilovic;P. Pagano;V. Polito;I. De Moortel;D. Nóbrega-Siverio;T. Van Doorsselaere;A. Petralia;M. Asgari-Targhi;P. Boerner;M. Carlsson;G. Chintzoglou;A. Daw;E. DeLuca;L. Golub;Takuma Matsumoto;I. Ugarte-Urra;S. McIntosh
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作者：
B. De Pontieu;P. Testa;J. Martínez-Sykora;P. Antolin;K. Karampelas;V. Hansteen;M. Rempel;M. Cheung;F. Reale;S. Danilovic;P. Pagano;V. Polito;I. De Moortel;D. Nóbrega-Siverio;T. Van Doorsselaere;A. Petralia;M. Asgari-Targhi;P. Boerner;M. Carlsson;G. Chintzoglou;A. Daw;E. DeLuca;L. Golub;Takuma Matsumoto;I. Ugarte-Urra;S. McIntosh
多狭缝太阳探测器（MUSE）是一个拟议的使命，由一个多狭缝极紫外（EUV）光谱仪（在171 nm、284 nm和108 nm三个光谱波段）和一个EUV背景成像仪（在195 nm和304 nm两个通带）组成。由于其创新的多光设计，MUSE将以高空间分辨率（≤0.“5）和时间分辨率（对于坐立凝视观测，分辨率低至0.5秒）提供前所未有的日冕光谱和成像诊断。通过获得四条明亮的EUV谱线的光谱，（Fe ix 171，Fe xv 284，Fe xix-Fe xxi 108）同时覆盖了大范围的过渡区和沿沿着37条狭缝的日冕温度，MUSE将首次“冻结”（以短至10秒的节奏）与光谱光栅的动态日冕等离子体的演变在一个广泛的尺度：从能量释放的空间尺度（≤0.″5）到大尺度（≤ 170″ × 170″）的大气响应。我们使用数值模拟来展示MUSE将如何在时空尺度（≤0.“5，≤20 s）上限制太阳大气的属性，以及最先进的驱动日冕加热，耀斑和日冕物质抛射（CME）的物理过程模型的大视野，做出区分和可检验的预测。我们描述了MUSE，单缝，高分辨率Solar-C EUVST摄谱仪，和地面观测站（DKIST等）之间的协同作用，以及MUSE由于所涉及的物理过程的多尺度性质而发挥的关键作用。在这第一篇论文中，我们专注于日冕加热机制。随附的一篇论文着重于耀斑和日冕物质抛射。
The Multi-slit Solar Explorer (MUSE) is a proposed mission composed of a multislit extreme ultraviolet (EUV) spectrograph (in three spectral bands around 171 Å, 284 Å, and 108 Å) and an EUV context imager (in two passbands around 195 Å and 304 Å). MUSE will provide unprecedented spectral and imaging diagnostics of the solar corona at high spatial (≤0.″5) and temporal resolution (down to ∼0.5 s for sit-and-stare observations), thanks to its innovative multislit design. By obtaining spectra in four bright EUV lines (Fe ix 171 Å, Fe xv 284 Å, Fe xix–Fe xxi 108 Å) covering a wide range of transition regions and coronal temperatures along 37 slits simultaneously, MUSE will, for the first time, “freeze” (at a cadence as short as 10 s) 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) to the large-scale (∼170″ × 170″) atmospheric response. We use numerical modeling to showcase how MUSE will constrain the properties of the solar atmosphere on spatiotemporal scales (≤0.″5, ≤20 s) and the large field of view on which state-of-the-art models of the physical processes that drive coronal heating, flares, and coronal mass ejections (CMEs) make distinguishing and testable predictions. We describe the synergy between MUSE, the single-slit, high-resolution Solar-C EUVST spectrograph, and ground-based observatories (DKIST and others), and the critical role MUSE plays because of the multiscale nature of the physical processes involved. In this first paper, we focus on coronal heating mechanisms. An accompanying paper focuses on flares and CMEs.