Results 301 to 310 of about 1,216,409 (346)
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2005
We present the fundamental equations which govern the physics of quiescent solar prominences. The mechanical equilibrium of prominences is described by the equations of magneto-hydrostatics. The radiative properties of the structures have to be modelled by non-LTE equations.
Heinzel, P., Anzer, U.
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We present the fundamental equations which govern the physics of quiescent solar prominences. The mechanical equilibrium of prominences is described by the equations of magneto-hydrostatics. The radiative properties of the structures have to be modelled by non-LTE equations.
Heinzel, P., Anzer, U.
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Solar Physics, 1972
This colloquium on solar prominences - the first ever held - has shown that a major part of activity in prominence research in recent years concentrated on both observation and computation of the magnetic conditions which were found to play a crucial role for the development and the maintainance of prominences.
Anton Bruzek, Max Kuperus
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This colloquium on solar prominences - the first ever held - has shown that a major part of activity in prominence research in recent years concentrated on both observation and computation of the magnetic conditions which were found to play a crucial role for the development and the maintainance of prominences.
Anton Bruzek, Max Kuperus
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Resolving the solar prominence/filament paradox using the magnetic Rayleigh–Taylor instability
Nature Astronomy, 2022J. Jenkins, R. Keppens
semanticscholar +1 more source
Kinematics of solar prominences
Solar Physics, 1983Using a 16-mm film recorded by R. B. Dunn at Sacramento Peak Observatory with a 15-inch coronagraph, we have studied motions of three solar prominences from the kinematic point of view. We applied three methods proposed earlier (Billings and Pecker, 1954; Palus, 1972; Makhmudov et al., 1980) to three prominences of the film.
J.L. Ballester, J. Kleczek
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A Complex Diagnostic of Solar Prominences
Solar Physics, 1996We use the polarimetric and intensity measurements of Hα and Hel D3 lines in solar prominences to derive the true geometrical thickness for several quiescent promi-nences. The electron densities, derived from the collisional depolarization in Hα by Bommier et al. (1994), are used to evaluate the thickness from the emission measure. The emission measure
Heinzel, P., Bommier, V., Vial, J.
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Magneto-thermal convection in solar prominences
Nature, 2011Coronal cavities are large low-density regions formed by hemispheric-scale magnetic flux ropes suspended in the Sun's outer atmosphere. They evolve over time, eventually erupting as the dark cores of coronal mass ejections. Although coronal mass ejections are common and can significantly affect planetary magnetospheres, the mechanisms by which cavities
Thomas, Berger +8 more
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Modern Observations of Solar Prominences
Solar Physics, 1985We review observational studies of solar prominences with some reference to theoretical understandings. We lay emphasis on the following findings: (1) An important discovery was made by Leroy, Bommier, and Sahal-Brechot concerning the direction of the magnetic field inside some high-altitude, high-latitude prominences, where the field vector points in ...
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Prominences and Solar Activity
International Astronomical Union Colloquium, 1979The following subjects were discussed:(1)Filament activation(2)Post-flare loops.(3)Surges and sprays.(4)Coronal transients.(5)Disk vs. limb observations.(6)Solar cycle variations of prominence occurrence.(7)Active prominences patrol service.Of all these items, (1) and (2) were discussed in most detail and we also pay most attention to them in this ...
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Condensation of solar prominences
Vistas in Astronomy, 1965Abstract Many solar prominences are formed by condensation of coronal gases. Recent progress in our knowledge of the condensation process is surveyed. Some open problems are discussed in the concluding section.
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RMHS Modeling of Solar Prominences
AIP Conference Proceedings, 2009In 1976 J. Heasley and D. Mihalas published a seminal paper devoted to the modeling of solar prominences. They applied their stellar atmospheric code based on the novel complete linearization method to model the radiation‐magnetohydrostatic (RMHS) coupling in prominences, to solve the multilevel transfer problem for a mixture of hydrogen and helium and
P. Heinzel +4 more
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