一种由阿尔文波驱动的自洽太阳日冕加热模型
A self-consistent solar coronal heating model by Alfvenic waves
AI总结：
该研究通过三维辐射磁流体力学模拟证实，太阳日冕主要由阿尔文波湍流主导的AC加热，占比至少80%，支持空间天气研究中AWSoM等阿尔文波湍流模型的应用。
AI中文摘要：
阿尔文波普遍存在于太阳大气中，被认为在日冕加热中发挥关键作用，这类加热被归类为交流电（AC）加热，与和准静态磁力线编织相关的直流电（DC）加热形成对比。AC加热与DC加热的相对重要性取决于光球驱动源的细节以及磁场的构型。此外，即便AC加热占主导，学界已提出多种波耗散机制，但哪种机制占主导仍不明确，因为其效率取决于等离子体可压缩性和密度不均匀性。为解决这些问题，我们开展了从上层对流区延伸至日冕的日冕环的三维辐射磁流体力学（MHD）模拟，该模拟自洽地捕获了诸多相关物理过程。我们发现日冕主要由AC加热，其中阿尔文波湍流是主要贡献源，在本次模拟中占整个日冕加热的至少80%。我们的结果有力支持在空间天气和恒星活动研究中采用基于阿尔文波湍流的模型，例如阿尔文波太阳模型（AWSoM）和球外磁流体力学算法（MAS）。
英文摘要：
Alfvenic waves are prevalent throughout the solar atmosphere and are believed to play an essential role in coronal heating, classified as alternating current (AC) heating in contrast to direct current (DC) heating associated with quasi-static magnetic field line braiding. The relative importance of AC versus DC heating depends on the details of the photospheric driver and on the configuration of the magnetic field. Moreover, even if AC heating prevails, several wave dissipation mechanisms have been proposed, and which of them dominates remains unclear, as its efficiency depends on plasma compressibility and density inhomogeneity. We address these issues by performing three-dimensional radiative magnetohydrodynamic (MHD) simulations of a coronal loop spanning from the upper convection zone to the corona, which self-consistently capture many relevant physical processes. We find that the corona is predominantly heated by AC heating, with Alfven wave turbulence providing the primary contribution, accounting for at least 80% of the entire coronal heating in the present simulation. Our results strongly support the use of Alfven wave turbulence-based models employed in space weather and stellar activity research, such as the Alfven Wave Solar Model (AWSoM) and the Magnetohydrodynamic Algorithm outside a Sphere (MAS).
