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Nature, 1942
THE difficulties which have so far been experienced in working out a physical theory of the solar corona (vide Rosseland, “Theoretical Astrophysics”, Chap. 14) have apparently been increased by the discovery of Grotrian and Edlen that many of these lines are due to forbidden transitions of highly stripped atoms of iron and nickel having the ...
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THE difficulties which have so far been experienced in working out a physical theory of the solar corona (vide Rosseland, “Theoretical Astrophysics”, Chap. 14) have apparently been increased by the discovery of Grotrian and Edlen that many of these lines are due to forbidden transitions of highly stripped atoms of iron and nickel having the ...
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Nature, 1966
Physics of the Solar Corona By I. S. Shklovskii. Second edition. Translated by L. A. Fenn. Translation edited by A. Beer. Additional material translated and edited by A. J. Meadows. (International Series of Monographs on Natural Philosophy, Vol. 6.) Pp. x + 475. (London and New York: Pergamon Press, Ltd., 1965.) 120s. net.
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Physics of the Solar Corona By I. S. Shklovskii. Second edition. Translated by L. A. Fenn. Translation edited by A. Beer. Additional material translated and edited by A. J. Meadows. (International Series of Monographs on Natural Philosophy, Vol. 6.) Pp. x + 475. (London and New York: Pergamon Press, Ltd., 1965.) 120s. net.
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Eclipse Instrumentation for the Solar Corona
Applied Optics, 1970The expedition of the Harvard College Observatory, the Smithsonian Astrophysical Observatory, and the National Geographic Society to Miahuatlán, Mexico, to observe the total solar eclipse of 7 March 1970, is described. Instrumentation included a coronal spectrograph, television cameras recording on videotape, telescopes for photography of coronal ...
D H, Menzel, J M, Pasachoff
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2003
The solar corona is an extremely hot (106 K or about 0.1 keV), almost fully ionised plasma which extends from a few thousand km above the Sun’s visible surface or photosphere (6000 K) to where it freely expands into the solar system as the solar wind.
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The solar corona is an extremely hot (106 K or about 0.1 keV), almost fully ionised plasma which extends from a few thousand km above the Sun’s visible surface or photosphere (6000 K) to where it freely expands into the solar system as the solar wind.
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Alfvén Waves in the Solar Corona
Science, 2007Alfvén waves, transverse incompressible magnetic oscillations, have been proposed as a possible mechanism to heat the Sun's corona to millions of degrees by transporting convective energy from the photosphere into the diffuse corona. We report the detection of Alfvén waves in intensity, line-of-sight velocity, and linear polarization images of the ...
S, Tomczyk +6 more
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1988
The structure of the quiet solar corona is considered, excluding the effect of magnetic active regions. Starting with a simple one-dimensional geometry, models are derived both from ab initio theory and from analysis of spectral line intensities. To overcome the inconsistencies which arise, account is taken progressively of two-dimensional effects; the
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The structure of the quiet solar corona is considered, excluding the effect of magnetic active regions. Starting with a simple one-dimensional geometry, models are derived both from ab initio theory and from analysis of spectral line intensities. To overcome the inconsistencies which arise, account is taken progressively of two-dimensional effects; the
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Optical Obsdervations of the Solar Corona
Space Science Reviews, 1982The history of optical observations of the solar corona is traced through the development of lour topics: the observation of naturally occurring total solar eclipses, the discovery of forbidden emission lines in the solar corona, the development of narrow spectral bandpass observing techniques, and the invention of the coronagraph.
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Astrophysics and Space Science, 1996
The solar corona, and the coronae of solar-type stars, consist of a low-density magnetized plasma at temperatures exceeding 106 K. The primary coronal emission is therefore in the UV and soft x-ray range. The observed close connection between solar magnetic fields and the physical parameters of the corona implies a fundamental role for the magnetic ...
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The solar corona, and the coronae of solar-type stars, consist of a low-density magnetized plasma at temperatures exceeding 106 K. The primary coronal emission is therefore in the UV and soft x-ray range. The observed close connection between solar magnetic fields and the physical parameters of the corona implies a fundamental role for the magnetic ...
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