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high-speed solar wind stream.
Such storms often follow from the interaction of a fast solar wind stream or an interplanetary magnetic cloud.
Electrons, protons, and other charged particles in the solar wind stream from the sun's outer atmosphere, or corona, at speeds of about 1.5 million kilometers per hour.
In response to a powerful/large coronal mass ejection (CME) or high-speed solar wind stream, an intense storm with Dst decreasing down to < −100 nT can occur.
They are designed to guide the on-coming wind stream to an optimum flow angle before it interacts with the rotor blades.
Particular emphasis is placed on the evolution of the solar wind stream structure, and its effect on the energetic particle fluxes observed at Ulysses.
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All the so-called people, wind streaming from their faces.
The pair could sense not only the magnetic field carried in the solar wind streaming off the Sun, but their interactions with it as they moved.
At that spot, says Hester, a violent but steady wind streaming from the pulsar careens into a frothy shock front of disordered electrons.
This paper introduces an investigation of shocklike soliton or small amplitude Double Layers (DLs) in a collisionless plasma, consisting of positive and negative ions, nonthermal electrons, as well as solar wind streaming protons and electrons.
In addition, majority of substorms occurred during low or moderate solar wind streams.
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