Results 151 to 160 of about 860 (182)
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Solar Coronal Heating by Dissipating Current Sheets
Physica Scripta, 2004It is shown that the lower-hybrid turbulence produced by the lower-hybrid-drift wave instability at current sheets can heat electrons and ions in the solar corona.
R. Bingham, P. K. Shukla, D. S. Spicer
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To the problem of solar coronal heating
Astronomy Letters, 2007We consider the adequacy of various solar coronal heating models. We show that the correlation between the intensity of the coronal Fe XIV 530.5 nm green line and the calculated magnetic field strength in the solar corona can be a useful tool for this purpose.
O. G. Badalyan, V. N. Obridko
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Solar Coronal Heating by Magnetic Flux Interaction
1994A Converging Flux Model for heating X-ray bright points (and possibly coronal loops and coronal holes) is proposed which also accounts for the cancelling magnetic features that are usually observed to be present in the photosphere below bright points.
E. R. Priest +2 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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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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Scaling of heating rates in solar coronal loops
Nature, 1995THE gas of the solar corona is at a temperature of several million degrees, orders of magnitude hotter than the underlying photosphere. The nature of the physical process that heats the solar corona (and the coronae of solar-type stars more generally) has been a long-standing puzzle.
James A. Klimchuk, Lisa J. Porter
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Learning about coronal heating from solar wind observations
Physics of Plasmas, 2005Vlasov theory describing the interaction of Alfvén-cyclotron fluctuations and ions in the collisionless solar wind predicts that alpha particles should be strongly scattered perpendicular to the background magnetic field when the alpha/proton relative velocity vαp is negative or has a sufficiently small positive value relative to the Alfvén speed vA ...
S. Peter Gary +2 more
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Solar flares, microflares, nanoflares, and coronal heating
Solar Physics, 1991Solar flare occurrence follows a power-law distribution against total flare energy W: dN/dW ∼ W−α with an index α ∼ 1.8 as determined by several studies. This implies (a) that microflares must have a different, steeper distribution if they are energetically significant, and (b) there must be a high-energy cutoff of the observed distribution.
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Solar coronal heating and weak fast shocks
2002It is suggested that protons and minor ions in the solar corona can be heated and accelerated by fast shocks.
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