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The Solar Chromosphere
A young boy, angry because his family is moving again, begins to play with puppets rather than make new friends.
The Solar Chromosphere and Corona: Quiet Sun
The widespread tendency in solar physics to divide the solar atmosphere into separate layers and to distinguish phenomena of solar activity from phenomena of the quiet Sun emphasizes the wide ranging diversity of physical conditions and events occurring in the solar atmosphere. This diversity spans the range from a neutral, essentially quiescent atmosphere to a highly ionized, violently convective atmosphere; from a domain in which magnetic field effects are unimportant to a domain in which the magnetic pressure exceeds the gas pressure, and from a domain in which the particle motions are Maxwellian to a domain in which an appreciable fraction of the particles is accelerated to relativistic ...
The Temperature Distribution in the Solar Chromosphere
A new approximate method is developed for calculating the temperature distribution in an atmosphere where local mechanical-energy dissipation is balanced by local net radiative loss in one or more spectral lines for which the atmosphere is optically thick. The method uncouples the equations of radiative transfer for the individual spectral lines from the energy-conservation equation and from each other. This permits a solution of each individual transfer equation for the radiation field in each line. These results, used in the energy-conservation equation, yield the temperature distribution if the optical depth ratio of the spectral lines at each point is known. The method is applied to selected strong resonance lines in the solar chromosphere.
The Solar Transition Region
The solar transition region, which spans the temperature range from about 20,000 to 1,000,000 K, separates the chromosphere from the corona. All the energy that heats the corona and powers the solar wind must pass through this part of the solar atmosphere. This book summarizes recent ultraviolet and extreme ultraviolet observations of the transition region, the empirical models derived from them, and the physical models that try to explain both the observations and the empirical models. The observational focus is on quiet solar transition region observations made with Skylab and subsequent rocket and satellite experiments. The book also presents a unified discussion of the analysis of ultraviolet and extreme ultraviolet spectroscopic data, including the determination of the emission measure and density and temperature diagnostics. This will be useful to astrophysicists who are confronting high-resolution ultraviolet and extreme ultraviolet data from astrophysical plasmas for the first time.
Mechanisms of Chromospheric and Coronal Heating
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.
Stellar Chromospheres
Conference on stellar chromospheres and their compositions.
Stellar Chromospheres
Conference on stellar chromospheres and their compositions.
