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Then, I describe the forward modeling pipeline for predicting time-dependent, multi-wavelength emission over an entire active region. In particular, the focus of this work is constraining the frequency with which nanoflares occur on a given magnetic field line in non-flaring active regions.įirst, I give an introduction to the structure of the solar atmosphere and coronal heating, discuss the hydrodynamics of coronal loops, and provide an overview of the important emission mechanisms in a high-temperature, optically-thin plasma. In this thesis, I use a hydrodynamic model of the coronal plasma combined with a sophisticated forward modeling approach and machine learning classification techniques to predict signatures of nanoflare heating and compare these predictions to real observational data.
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However, a direct detection of heating by nanoflares has proved difficult due to their faint, transient nature and as such, properties of this proposed heating mechanism remain largely unconstrained. Nanoflares, small-scale bursts of energy likely resulting from the frequent reconnection of twisted magnetic field lines, have long been proposed as a candidate for heating the non-flaring corona, especially in areas of high magnetic activity. While it is generally agreed that the continually stressed coronal magnetic field plays a role in producing these million-degree temperatures, the exact mechanism responsible for transporting this stored energy to the coronal plasma is yet unknown. This so-called "coronal heating problem" has occupied the field of solar astrophysics for over seventy years and is one of the most important open questions in astronomy as a whole. The solar corona, the outermost layer of the Sun's atmosphere, is heated to temperatures in excess of one million Kelvin, nearly three orders of magnitude greater than the surface of the Sun.