Structure of the solar atmosphere: a radio perspective
TL;DR: In this paper, the authors present a review of the physical processes that determine solar radio emission and link the radio domain with the rest of the electromagnetic spectrum, which is necessary to understand the solar radio emissions.
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Abstract: Solar radio emission has been providing information about the Sun for over half a century. In order to fully exploit this information, one needs to have a broader view of the solar atmosphere, which cannot be provided by radio observations alone. The purpose of this review is to present this background information, which is necessary to understand the physical processes that determine the solar radio emission and to link the radio domain with the rest of the electromagnetic spectrum.
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Citations
Radio Measurements of the Magnetic field in the Solar Chromosphere and the Corona
C. E. Alissandrakis,Dale E. Gary +1 more
TL;DR: In this paper, the magnetic field effects on radio emission produced by incoherent emission mechanisms (free-free, gyroresonance and gyrosynchrotron processes) are discussed.
The Solar Atmosphere
TL;DR: In this article, the authors investigated the appearance of the spectrum which appeared on the bulb of the focal thermometer after shutting out the rays from the photosphere during the experiments and concluded that its extent and position suggest that the depth of the solar atmosphere far exceeds the limits hitherto assumed.
Characterization and formation of on-disk spicules in the Ca II K and Mg II k spectral lines.
TL;DR: In this paper, the authors characterize type-II spicules in Ca II K 3934\AA using the CHROMIS instrument at the Swedish 1m Solar Telescope and find that their line formation is dominated by opacity shifts with the K$3}$ minimum best representing the velocity of the spicule.
References
Direct evidence for neutrino flavor transformation from neutral current interactions in the Sudbury Neutrino Observatory
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TL;DR: Observations of neutral-current nu interactions on deuterium in the Sudbury Neutrino Observatory are reported, providing strong evidence for solar nu(e) flavor transformation.
Structure of the solar chromosphere. III. Models of the EUV brightness components of the quiet sun
TL;DR: In this paper, the solution of the non-LTE optically thick transfer equations for hydrogen, carbon, and other constituents to determine semi-empirical models for six components of the quiet solar chromosphere was investigated.
2.4K
Nanoflares and the solar X-ray corona
TL;DR: In this paper, it was shown that the X-ray corona is created by the dissipation at the many tangential discontinuities arising spontaneously in the bipolar fields of the active regions of the sun as a consequence of random continuous motion of the footpoints of the field in the photospheric convection.
1.9K
Magnetic Fields and the Structure of the Solar Corona. I: Methods of Calculating Coronal Fields
TL;DR: In this paper, several different mathematical methods are described which use the observed line-of-sight component of the photospheric magnetic field to determine the magnetic field of the solar corona in the current-free approximation.
1.1K
On Solving the Coronal Heating Problem
TL;DR: The question of what heats the solar corona remains one of the most important problems in astrophysics as mentioned in this paper, and finding a definitive solution involves a number of challenging steps, beginning with an identification of the energy source and ending with a prediction of observable quantities that can be compared directly with actual observations.
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