Results 181 to 190 of about 1,498,055 (202)

Solar coronal heating by magnetosonic waves

Monthly Notices of the Royal Astronomical Society, 2001
Solar 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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Coronal Heating and Solar Wind

1965
We have now to consider the heat carried mechanically in the chromosphere and corona and hope to explain in this way the heating of these two regions. It can be said that the present theories give a picture of the temperature in the chromosphere and corona which show all the main features of the observed temperature distribution.
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Nonlinear wave heating of solar coronal loops.

Astronomy and Astrophysics, 1997
The 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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Solar Coronal Heating by Dissipating Current Sheets

Physica Scripta, 2004
It 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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Effect of areal expansion and coronal heating on the solar wind

Space Science Reviews, 1994
Empirical studies have shown that the solar wind speed at Earth is inversely correlated with the areal expansion rate of magnetic flux tubes near the Sun. Recent model calculations that include a self-consistent determination of the coronal temperature allow one to understand the physical basis of this relationship; they also suggest why the solar wind
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Intermittent heating in a model of solar coronal loops

Solar Physics, 2000
X-ray and EUV observations of the solar corona reveal a very complex and dynamic environment where there are many examples of structures that are believed to outline the Sun's magnetic field. In this present study, the authors investigate the temporal response of the temperature, density and pressure of a solar coronal plasma contained within a ...
R.W. Walsh, S. Galtier
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Solar Coronal Heating by Magnetic Flux Interaction

1994
A 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, C. E. Parnell, G. J. Rickard   +2 more
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Solar coronal heating and weak fast shocks

2002
It is suggested that protons and minor ions in the solar corona can be heated and accelerated by fast shocks.
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Coronal heating and solar wind acceleration by turbulence

2006
Observations such as Spartan and SOHO UVCS have challenged ideas for the acceleration of the solar wind by constraining models to produce >1.5 Million K protons, several hundred km~s-1 radial outflows, and >700 km~s-1 terminal speeds in the wind emanating from polar coronal holes, with coronal electrons remaining cooler than protons.
VERDINI, ANDREA, VELLI, MARCO, W. H. Matthaeus   +2 more
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HEATING CORONAL HOLES AND ACCELERATING THE SOLAR WIND

1992
The special energy requirements of a coronal hole combined with current knowledge of the limited dissipation of Alfven and fast mode MHD waves in the solar corona suggest a unique source of heat for the coronal hole. The near coronal hole requires approximately 3 - 4 x 10 exp 5 ergs/sq cm s, which can come only from the fluid jets, fast particles, and ...
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