Titlebook: Solar-Terrestrial Physics; Principles and Theor R. L. Carovillano,J. M. Forbes Conference proceedings 1983 D. Reidel Publishing Company, Do

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endoscopy

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Generation of Solar Magnetic Fields Igeneral because the sun is by no means an isolated body. In these lectures I will talk about the properties of magnetic fields that allow them to destroy themselves remarkably rapidly, producing solar activity, stellar activity, geomagnetic activity, and so forth. It might be called the birth and de

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manifestation

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Heating of the Outer Solar Atmosphere IIe closed; they come out at one point and reenter at another (Figure 1). The foot points of the lines of force are continually being shuffled around at random, twisting the fields above. At the end of the previous lecture we considered an idealized problem. It consists of an initially uniform field e

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Hydromagnetic Waves, Turbulence, and Collisionless Processes in the Interplanetary Medium of milliseconds. Most of the power in interplanetary waves and turbulence lies at hydromagnetic scales. These fluctuations are normally of large amplitude, containing enough energy to affect solar and galactic cosmic rays, and may be the remnants of a coronal turbulence field powerful enough to pla

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The Acceleration of Energetic Particles in the Solar Windefly. Statistical accleration in both Alfven and magnetosonic turbulence is considered, but it is argued that neither may be of particular importance in the solar wind. Shock acceleration is illustrated with the case of acceleration at the forward and reverse shocks which bound corotating interactio

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Large-Scale Morphology of the Magnetospheretic fields. This chapter surveys the principal large- scale structures associated with the interaction between the solar wind and the earth, introduces the various terms by which they are known, and sketches their physical properties and their theoretical interpretation if there is a widely accepted