Results 31 to 40 of about 50 (47)
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Interdependence of solar wind models and solar wind observations
AIP Conference Proceedings, 1997A brief overview of the observations in the inner corona is presented together with three different solar wind models. It is shown that the very high flow speeds derived from the observations in the inner corona can be modeled if either the proton temperature is extremely high, or if there exists a mechanism that adds momentum to the flow much closer ...
Nancy Brickhouse, Ruth Esser
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Space Science Reviews, 1983
Some advances in the hydrodynamical large-scale theory, on the one hand, and in the kinetic theory, on the other hand, of the solar wind are reviewed. For brevity, we sketch the general frame, point out the problems and approaches and then illustrate by a few examples the ways in which progress has been achieved during the past four years.
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Some advances in the hydrodynamical large-scale theory, on the one hand, and in the kinetic theory, on the other hand, of the solar wind are reviewed. For brevity, we sketch the general frame, point out the problems and approaches and then illustrate by a few examples the ways in which progress has been achieved during the past four years.
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1998
The first evidence of the solar wind was provided through observations of comet tail deflections by L. Biermann in 1951. A cometary ion tail is oriented along the difference between the cometary and solar wind velocities, whereas the dust tail is in the antisunward direction; the ion tail directions demonstrated the existence of an outflow of ionized ...
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The first evidence of the solar wind was provided through observations of comet tail deflections by L. Biermann in 1951. A cometary ion tail is oriented along the difference between the cometary and solar wind velocities, whereas the dust tail is in the antisunward direction; the ion tail directions demonstrated the existence of an outflow of ionized ...
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Space Science Reviews, 1996
The solar wind carves a cavity in the flow of interstellar H atoms through the solar system by charge-exchange ionization. The resulting Ly-α sky pattern depends on the latitude distribution of the solar wind flux and velocity. We review how the solar wind characteristics (mass flux latitude distribution) can be retrieved from Ly-α observations ...
Bertaux, Jean-Loup +2 more
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The solar wind carves a cavity in the flow of interstellar H atoms through the solar system by charge-exchange ionization. The resulting Ly-α sky pattern depends on the latitude distribution of the solar wind flux and velocity. We review how the solar wind characteristics (mass flux latitude distribution) can be retrieved from Ly-α observations ...
Bertaux, Jean-Loup +2 more
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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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Solar activity and the solar wind
Reviews of Geophysics, 1979The availability of in situ solar wind observations from the complete sunspot cycle 20 (1964–1976) suggests an examination of the changes in the character of the solar wind related to the solar cycle and comparison of these observed changes with those expected from earlier studies of solar‐terrestrial physics.
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1990
Some 4.56 billion years ago, out of the gravitational collapse of a cloud in the interstellar medium with angular momentum L, a rotating star — the Sun — was formed, and began to burn hydrogen into helium and heavier nuclei. A gaseous disc in the plane orthogonal to L developed; its chemical composition, initially the same as in the solar photosphere ...
Bruno Bertotti +2 more
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Some 4.56 billion years ago, out of the gravitational collapse of a cloud in the interstellar medium with angular momentum L, a rotating star — the Sun — was formed, and began to burn hydrogen into helium and heavier nuclei. A gaseous disc in the plane orthogonal to L developed; its chemical composition, initially the same as in the solar photosphere ...
Bruno Bertotti +2 more
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Diagnostics of the Solar Wind Plasma
2009The solar wind is a fully ionized plasma, coming from the outer atmosphere of the Sun, the so-called solar corona, which expands as a supersonic flow into the interplanetary medium [55]. The first observations indicating that the Sun might be emitting a wind were made by Biermann in 1946 of comet tails [1], which are observed to point away from the Sun.
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2019
The Sun continuously expels a fraction of its own mass in the form of a steadily accelerating outflow of ionized gas called the “solar wind.” The solar wind is the extension of the Sun’s hot (million-degree Kelvin) outer atmosphere that is visible during solar eclipses as the bright and wispy corona.
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The Sun continuously expels a fraction of its own mass in the form of a steadily accelerating outflow of ionized gas called the “solar wind.” The solar wind is the extension of the Sun’s hot (million-degree Kelvin) outer atmosphere that is visible during solar eclipses as the bright and wispy corona.
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