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This book reflects on 8 decades of research on one of the longest-standing unsolved problems in modern astrophysics: why does the Sun form a hot corona? The authors give a critical overview of the field and offer suggestions on how to bridge the chasm between what we can measure, and what we can calculate. They go back to basics to explain why the problem is difficult, where we have made progress and where we have not, to help the next generation of scientists devise novel techniques to crack such a long-lasting problem. A way forward is formulated centered around refutation, using Bayesian methods to propose and to try to reject hypotheses and models, and avoiding seduction by ``confirmation bias’’. This book is aimed at physicists, students and researchers interested in understanding, learning from and solving the coronal heating problem, in an era of new dedicated facilities such as the Parker Solar Probe and the Daniel K. Inouye Solar Telescope. The book will appeal to those interested in understanding research methods and how they are changing in the modern academic environment, particular in astrophysics and Earth sciences where remote sensing is essential.
A thorough introduction to solar physics based on recent spacecraft observations. The author introduces the solar corona and sets it in the context of basic plasma physics before moving on to discuss plasma instabilities and plasma heating processes. The latest results on coronal heating and radiation are presented. Spectacular phenomena such as solar flares and coronal mass ejections are described in detail, together with their potential effects on the Earth.
This volume is dedicated to the Solar Dynamics Observatory (SDO), which was launched 11 February 2010. The articles focus on the spacecraft and its instruments: the Atmospheric Imaging Assembly (AIA), the Extreme Ultraviolet Variability Experiment (EVE), and the Helioseismic and Magnetic Imager (HMI). Articles within also describe calibration results and data processing pipelines that are critical to understanding the data and products, concluding with a description of the successful Education and Public Outreach activities. This book is geared towards anyone interested in using the unprecedented data from SDO, whether for fundamental heliophysics research, space weather modeling and forecasting, or educational purposes. Previously published in Solar Physics journal, Vol. 275/1-2, 2012. Selected articles in this book are published open access under a CC BY-NC 2.5 license at link.springer.com. For further details, please see the license information in the chapters.
This advanced textbook reviews the complex interaction between the Sun's plasma atmosphere and its magnetic field.
It has been known since the 1930s that the solar corona is hundreds of times hotter than the solar photosphere. Numerous theoretical models have since been proposed to explain what has become known as the coronal heating problem. These models are broadly cate- gorised as either wave heating (AC) or magnetic reconnection (DC). In this thesis aspects of both AC and DC heating models are investigated using analytical and numerical tech- niques. The dominant AC heating model, known as phase mixing, proposes that magnetic Alfven waves, generated at the photosphere, dissipate in the corona due to inhomoge- neous coronal structures. In this work corrected analytical solutions are presented for the enhanced phase mixing of linear Alfven waves in divergent and stratified coronal struc- tures. Numerical simulations are used to confirm the validity of these analytical solutions. Further numerical simulations investigate the magnitude and location of the wave dissi- pation. It is found that the enhanced phase mixing of 0.1 Hz Alfven waves can fulfil the coronal heating energy requirement. The DC heating models propose that eruptions of photospheric plasma, known as so- lar flares, are initiated by the reconnection of magnetic fields. These frequently observed flares release significant quantities of stored magnetic energy over a wide range of spa- tial scales, heating the surrounding plasma. In this work the magnetic reconnection of coalescing chromospheric current loops is investigated using two-fluid numerical simula- tions. It is found that the rate of the magnetic reconnection, and hence energy release, is strongly affected by the initial local plasma conditions. Finally, a model is proposed to explain the recently discovered penumbral micro-jets, based on the interaction of coalescing current loops with background magnetic flux tubes. Bidirectional jets and significant proton heating are observed in numerical simulations of the proposed model.
One of the great problems of astrophysics is the unanswered question about the origin and mechanism of chromospheric and coronal heating. Just how these outer stellar envelopes are heated is of fundamental importance, since all stars have hot chromospheric and coronal shells where the temperature rises to millions of degrees, comparable to the temperatures in the stars' cores. Here for the first time is a comprehensive inventory of the proposed chromospheric and coronal heating theories. The proposed heating processes are critically compared, and the observational evidence for the various mechanisms is reviewed. This is essential reading for all those working in such fields as stellar activity, radio and XUV emission, rotation, and mass loss, for whom a detailed and consistent presentation of our knowledge of chromospheric and coronal heating mechanisms is urgently needed.
A self-contained introduction to magnetohydrodynamics with emphasis on nonlinear processes.
The book provides a comprehensive overview of the eruptive and wave phenomena in the solar atmosphere. One of the ongoing problems in solar physics is the heating of the solar corona. Currently there is a competition between two mechanisms in explaining the heating, i.e., dissipation of energy by waves and small scale frequent coronal magnetic reconnection. However, some studies indicate this may be a joint effect of these two possible mechanisms. Kelvin-Helmholtz Instability (KHI) of propagating magnetohydrodynamic modes in solar flowing structures plays an important role in the solar atmosphere. It can trigger the onset of wave turbulence leading to effective plasma heating and particle acceleration. KHI is a multifaceted phenomenon and the purpose of this book is to illuminate its (instability) manifestation in various solar jets like spicules, dark mottles, surges, macrospicules, Extreme Ultraviolet (EUV) and X-ray jets, as well as rotating, tornado-like, jets, solar wind, and coronal mass ejections. The modeling of KHI is performed in the framework of ideal magnetohydrodynamics. The book consists of 12 chapters and is intended primarily for advanced undergraduate and postgraduate students, as well as early career researchers.