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2009
Looking at the solar photosphere, we see the top of the convection zone in the form of granulation: Hot gas rising from the solar interior as part of the energy transport process reaches a position where the opacity is no longer sufficient to prevent the escape of radiation.
V.H. Hansteen, M. Carlsson
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Looking at the solar photosphere, we see the top of the convection zone in the form of granulation: Hot gas rising from the solar interior as part of the energy transport process reaches a position where the opacity is no longer sufficient to prevent the escape of radiation.
V.H. Hansteen, M. Carlsson
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Solar Physics, 1973
The solar atmosphere is heated by a flux of mechanical waves propagating in one or more of the modes: acoustic, Alfven and gravitational.
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The solar atmosphere is heated by a flux of mechanical waves propagating in one or more of the modes: acoustic, Alfven and gravitational.
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2001
As a typical star, and the only one that can be spatially resolved by direct means, the study of the Sun has provided an insight into many of the fundamental processes taking place in stellar atmospheres, often at small scales. A prime example is magneto-convection or the formation of coronae and the consequent emission of copious amounts of X-rays. In
Solanki, S., Hammer, R.
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As a typical star, and the only one that can be spatially resolved by direct means, the study of the Sun has provided an insight into many of the fundamental processes taking place in stellar atmospheres, often at small scales. A prime example is magneto-convection or the formation of coronae and the consequent emission of copious amounts of X-rays. In
Solanki, S., Hammer, R.
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Turbulence in the Solar Atmosphere and Solar Wind
Space Science Reviews, 2010The objective of this review article is to critically analyze turbulence and its role in the solar atmosphere and solar wind, as well as to provide a tutorial overview of topics worth clarification. Although turbulence is a ubiquitous phenomenon in the sun and its heliosphere, many open questions exist concerning the physical mechanisms of turbulence ...
Petrosyan, A. +8 more
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1977
Abstract : We have studied the heating of the solar chromosphere and corona, and the propagation of acoustic waves through the transition region between the chromosphere and corona. In order to place an upper limit on the effectiveness of acoustic waves in heating, we have written and tested a computer program to accurately calculate the propagation ...
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Abstract : We have studied the heating of the solar chromosphere and corona, and the propagation of acoustic waves through the transition region between the chromosphere and corona. In order to place an upper limit on the effectiveness of acoustic waves in heating, we have written and tested a computer program to accurately calculate the propagation ...
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A Simplified Model Solar Atmosphere
Solar Physics, 1968A simplified representation of the temperature distribution in the solar photosphere is proposed: θ (τ 0) = θ 0 – θ 1 logτ 0. An expression is derived for the emergent continuous spectrum from the simple model. The limitations and applications of the simple model are discussed.
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Solar Magneto-Atmospheric Waves.
1975Abstract : The linearized theory of magneto-atmospheric waves (involving the combined restoring forces due to buoyancy, compressibility, and magnetic field) is developed for the case of a horizontal magnetic field which may vary with height. The convective stability of the basic atmosphere is considered, and it is shown that a nonuniform horizontal ...
null Jr +3 more
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