Titlebook: Basic Mechanisms of Solar Activity; V. Bumba,J. Kleczek Book 1976 International Astronomical Union 1976 Corona.Main sequence.Photosphere.R

integrated

https://doi.org/10.1007/978-94-010-1481-6Corona; Main sequence; Photosphere; Redshift; Solar; Sun; Sunspot

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1743-9213 Commission 10, we proposed to organize a Symposium which would stress the observational aspects of solar activity. It was our hope that such a Symposium might stimulate studies of those important problems in solar physics which for a long time had been neglected in overall scientific discussion. Alt

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Investigation of Coronal Rotation by the Spectroscopic Methodr region an intensive stream of coronal gas directed oppositely to the solar rotation was detected during the time interval 1969–1972. In the greater part of the latitude range, on average, the corona rotates more slowly in comparison with the solar atmosphere at the photospheric level.

observatory

Kai Maaz,Marko Neumann,Jürgen Baumerterent role or visibilility of structures in both polarities is discussed. The reflection of both main types of the longitudinal distribution of large-scale solar background magnetic fields (the 27-day, the 28–29-day successions, the ‘supergiant’ structures) in the interplanetary magnetic field distribution is also considered.

沉积物

https://doi.org/10.1007/978-3-476-04221-7oints. These observations suggest that surface motions do not exhibit the detailed flux redistribution expected in the random-walk diffusion of magnetic fields. It is suggested that the surface motions are only the reflection of magnetic field-convective motion interactions which occur deeper in the convection zone.

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https://doi.org/10.1007/978-3-7091-0050-9ntified in X-ray photographs are seen as small (5−10″) emission features in ground-based H. and Ca K spectroheliograms as well as in transition region lines observed in other Skylab instruments. Typical bright point temperatures are 1.5−2×10. K and typical densities are ~ 5×10. cm..