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AIP Conference Proceedings, 2007
We discuss the energy balance of the upper solar atmosphere and the solar wind, showing how the properties of the corona and solar wind are influenced by the three energy loss mechanisms available to the solar atmosphere; the solar wind, heat conduction, and radiation. We show that the Sun must have a corona with temperature of order 106 K irrespective
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We discuss the energy balance of the upper solar atmosphere and the solar wind, showing how the properties of the corona and solar wind are influenced by the three energy loss mechanisms available to the solar atmosphere; the solar wind, heat conduction, and radiation. We show that the Sun must have a corona with temperature of order 106 K irrespective
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2003
This chapter is intended to be an overview of the aspects of solar wind, with particular emphasis on the properties of the solar wind within about 1AU of the Sun. The topic is split into two parts on the basis of two types of solar wind flows, (i) quasi-stationary winds and (ii) transient flows.
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This chapter is intended to be an overview of the aspects of solar wind, with particular emphasis on the properties of the solar wind within about 1AU of the Sun. The topic is split into two parts on the basis of two types of solar wind flows, (i) quasi-stationary winds and (ii) transient flows.
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Journal of Research of the National Bureau of Standards, Section D: Radio Propagation, 1961
>Hydrodynamic expansion of the solar corona is the basis for solar corpuscular radiation. The quiet day coronal temperatures of 1 to 2 x 10/sup 6/ deg K yield a solar wind of several hundred km/sec and a density of 5 to 50 particles/cm/sup 3/ at the orbit of Earth.
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>Hydrodynamic expansion of the solar corona is the basis for solar corpuscular radiation. The quiet day coronal temperatures of 1 to 2 x 10/sup 6/ deg K yield a solar wind of several hundred km/sec and a density of 5 to 50 particles/cm/sup 3/ at the orbit of Earth.
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2000
Variations in the Earth’s magnetic field were first observed in the nineteenth century as a sudden increase (by about 10-3 G) followed by a slow decrease. These geomagnetic storms were sometimes found to occur one or two days after large solar flares, and further evidence for a link between the two phenomena came with the discovery of an 11-yr ...
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Variations in the Earth’s magnetic field were first observed in the nineteenth century as a sudden increase (by about 10-3 G) followed by a slow decrease. These geomagnetic storms were sometimes found to occur one or two days after large solar flares, and further evidence for a link between the two phenomena came with the discovery of an 11-yr ...
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Impact of siting ordinances on land availability for wind and solar development
Nature Energy, 2023Anthony Lopez +2 more
exaly
Optimizing wind/solar combinations at finer scales to mitigate renewable energy variability in China
Renewable and Sustainable Energy Reviews, 2020Laibao Liu, Rui Chang, Gang He
exaly