Results 191 to 200 of about 16,413 (221)
Statistical analysis and forecasting of solar wind parameters across solar cycles. [PDF]
Sci RepHe M, Zhu H.
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Searching for ultralight dark matter conversion in solar corona using Low Frequency Array data. [PDF]
Nat CommunAn H, Chen X, Ge S, Liu J, Luo Y.
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Solar coronal heating by magnetosonic waves
Monthly Notices of the Royal Astronomical Society, 2001Solar coronal heating by magnetohydrodynamic (MHD) waves is investigated. ultraviolet (UV) and X-ray emission lines of the corona show non-thermal broadenings. The wave rms velocities inferred from these observations are of the order of 25–60 km s−1. Assuming that these values are not negligible, we solved MHD equations in a quasi-linear approximation,
Pekunlu, ER, Cakirli, O, Ozetken, E
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Solar coronal heating by plasma waves
Journal of Plasma Physics, 2009AbstractThe solar coronal plasma is maintained at temperatures of millions of degrees, much hotter than the photosphere, which is at a temperature of just 6000 K. In this paper, the plasma particle heating based on the kinetic theory of wave–particle interactions involving kinetic Alfvén waves and lower-hybrid drift modes is presented.
Bingham, R. +3 more
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Alfvén waves in the solar polar coronal holes
AIP Conference Proceedings, 1999We study the variation of the line width and electron density as a function of height above two coronal holes from forbidden spectral lines of Si VIII. The spectra were obtained with the Solar Ultraviolet Measurements of Emitted Radiation spectrometer flown on the Solar and Heliospheric Observatory spacecraft.
Banerjee, D. +3 more
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Solar Coronal Heating via Alfvén Wave Turbulence
AIP Conference Proceedings, 2010A short review is given about the self‐consistent MHD model of solar coronal heating recently proposed by Bigot et al. (2008) in which the dynamical effect of the background magnetic field along a coronal structure is taken into account through exact results from Alfven wave turbulence.
B. Bigot +7 more
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Coronal heating and solar activity: The role of waves
Advances in Space Research, 1993Abstract Coronal heating and solar activity are manifestations of the complex interaction between the magnetic field and the photospheric plasma motions. As a result of such an interaction magnetohydrodynamic waves are generated: their dissipation may provide the basic physical mechanism to heat the corona.
EINAUDI G +2 more
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Solar coronal heating by high-frequency dispersive Alfvén waves
Solar Physics, 1999It is shown that high-frequency dispersive kinetic Alfven waves can cause significant electron heating in the solar corona. The heating is produced by collisionless electron Landau dissipation of the parallel electron current associated with high-frequency dispersive kinetic Alfven waves, which have a parallel electric field.
Shukla, P. +3 more
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Nonlinear wave heating of solar coronal loops.
Astronomy and Astrophysics, 1997The heating of magnetically closed structures (loops) in the solar corona by the resonant absorption of incident waves is studied by means of numerical simulations in the framework of nonlinear resistive magnetohydrodynamics (MHD). It is shown that the dynamics in the resonant layer is indeed very nonlinear for typical coronal parameters. The effect of
Poedts, S., Goedbloed, J.P.
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Observational Research on Solar Coronal Waves.
1976Abstract : An observational search has been made for intensity fluctuations associated with the wave motions that are thought to heat the corona. Brightness changes in the coronal green line (Fe XIV lambda 5303) and the coronal continuum were measured with the University of Hawaii's polarimeter at Mt. Haleakala.
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