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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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Cyclotron Heating of the Solar Corona
Astrophysics and Space Science, 1998A physical model of the solar transition region and corona is presented, in which plasma flows in rapidly-diverging coronal funnels and holes are described within the framework of a two-fluid model including wave-particle interactions. The ions are heated by wave dissipation and accelerated by the pressure gradient of high-frequency Alfven waves, which
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Parker Solar Probe Enters the Magnetically Dominated Solar Corona
Physical Review Letters, 2021Davin Larson +2 more
exaly
Radio Measurements of the Magnetic Field in the Solar Chromosphere and the Corona
Frontiers in Astronomy and Space Sciences, 2021Dale Gary
exaly
Waves and Turbulence in the Solar Corona
2004In the solar corona (and solar wind) waves and turbulence occur at all scales ranging from the particles’ gyroradii to the size of a solar radius (or even to an astronomical unit). A concise review of some new observations and theories of waves in the sun’s atmosphere and corona is given, with the focus being on coronal waves that are magnetically ...
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