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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.
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.
A Guide to the Solar Corona is specifically directed to the space scientist or engineer who is not a specialist in solar physics, but whose work requires a fairly detailed knowledge of the corona. It is hoped that the material may prove useful to most graduate students in astrophysics, while solar physicists may find some topics of interest and value to them. The book contains 12 chapters and begins with three descriptive chapters that provide the casual reader with a concept of the corona as it is evident through more or less direct observation. Topics covered include the development of coronal science, observational techniques, and observational aspects of the corona. The next chapter discusses methods of analyzing coronal data. Subsequent chapters present theoretical considerations as they are applicable to the corona. These combine theory with observation to provide a description of the various aspects of the corona. The final chapter is a combination of established ideas and speculation on the place of the corona in the universe.
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.
Second edition graduate level textbook giving an up-to-date treatment of our understanding of the solar corona.