KlappentextThis book comprises an excursion through space weather, a scientific topic in rapid growth and with growing impact and complications for technological societies. The emphasis of the present volume is on the origins of space weather: the Sun and the solar mind. Very much as the Sun`s electromagnetic radiation drives the Earth climate, our space weather is driven by the solar wind. This book addresses students and scientists working, or interested in, the field and provides a thorough introduction to the topic for those who wish to become acquainted with the basic solar physics at the origin of space weather.
Based on lectures given at a CNRS summer school in France, this book covers many aspects of stellar environments (both observational and theoretical) and offers a broad overview of the field. More specifically, Part I of the book focuses on the Sun, the properties of the ejected plasma, of the solar wind and on space weather. The second part deals with tides in planetary systems and in binary stellar systems, as well as with interactions in massive binary stars as seen by interferometry. Finally the chapters of Part III discuss the environments of young or evolved stars, stellar winds, agnetic fields and disks. With its broad approach the book will provide advanced students as well as researchers with a good overview of the environments of the Sun and the stars.
This volume of lecture notes brings together the knowledge on pulsations of the Sun and the stars, with a particular emphasis on recent observations and modelling, and on the influence of pulsations of other physical processes. The book begins with an extensive introduction to helioseismology. The solar cycle and gravity modes are discussed before the focus is widened from helioseismology to asteroseismology which is detailed in a series of specific chapters. Based on courses given at a graduate school, these tutorial lecture notes will be of interest and useful to a rather broad audience of scientists and students.
The Sun and stars rotate in di? erent ways and at di? erent velocity rates. The knowledge of how they rotate is important in understanding the formation and evolution of stars and their structure. The closest star to our Earth, the Sun, is a good laboratory to study in detail the rotation of a G star and allows to test new ideas and develop new techniques to study stellar rotation. More or less massive, more or lessevolved objects, however, can have averydi? erent rotation rate, structure and history. In recent years our understanding of the rotation of the Sun has greatly improved. The Sun has a well-known large-scale rotation, which can be m- sured thanks to visible features across the solar disk, such as sunspots, or via spectroscopy. In addition, several studies cast light on di? erential rotation in the convective zone and on meridional circulation in the radiative zone of the Sun. Even the rotation of the core of the Sun can now be studied thanks to various methods, such as dynamics of the gravitational moments and of course, helioseismology, through g-modes analysis. Moreover, the magnetic ? eld is strongly linked to the matter motions in the solar plasma. The solar magnetic ? eld can be measured only at the surface or in theupperlayers. Itistheproductoftheinternaldynamoorofthelocaldynamos if they exist – in any case magnetic ? eld and rotation cannot thus be separated.
Composed of a set of lectures and tutorial reviews, this book stems from a summer school devoted to the gravitational aspects of the sun and their geophysical consequences. Contribitions elaborate on the gravitational distortions of the sun which can be used to gain some knowledge of the sun's interior and surface phenomena but which also influences the sun's irradience and thus ultimately the earth's climate. Last but not least, it is shown that these small distortions constitute a formidable challenge to solar astrometry, and the final part of the book describes the observational difficulties in defining unequivocally the solar diameter.
Inhaltsverzeichnisto MHD.Magnetic Reconnection: Classical Aspects.Structuring of the Solar Plasma by the Magnetic Field.Structuring of the Magnetospheric Plasma by the Solar Terrestrial Interactions.Self-Consistent Kinetic Approach for Low Frequency and Quasi-static Electromagnetic Perturbations in Magnetic-Mirror Confined Plasmas.
