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A solar flare is a relatively intense, localized emission of electromagnetic radiation in the Sun's atmosphere.Flares occur in active regions and are often, but not always, accompanied by coronal mass ejections, solar particle events, and other eruptive solar phenomena.
These particles can escape the Sun's gravity because of their high energy. The solar wind is divided into the slow solar wind and the fast solar wind. The slow solar wind has a velocity of about 400 kilometres per second (250 mi/s), a temperature of 2 × 10 5 K and a composition that is a close
The solar wind also carries with it the Sun's magnetic field. This field will have either a North or South orientation. If the solar wind has energetic bursts, contracting and expanding the magnetosphere, or if the solar wind takes a southward polarization, geomagnetic storms can be expected.
This happens when the speed of the ICME in the frame of reference moving with the solar wind is faster than the local fast magnetosonic speed. Such shocks have been observed directly by coronagraphs [24] in the corona, and are related to type II radio bursts. They are thought to form sometimes as low as 2 R ☉ (solar radii).
The boundary separating the corona from the solar wind is called the Alfvén surface. At a distance of more than a few solar radii from the Sun, the solar wind reaches speeds of 250–750 km/s and is supersonic, [4] meaning it moves faster than the speed of fast magnetosonic waves.
A solar storm is a disturbance on the Sun, which can emanate outward across the heliosphere, affecting the entire Solar System, including Earth and its magnetosphere, and is the cause of space weather in the short-term with long-term patterns comprising space climate. [1] [2]
Apparently, had the experiment been performed even deeper underwater, the pressure would have been too intense and the egg would have eventually exploded on its own -- much like it did when the ...
Because the solar wind and the ISM are both fluid, the heliosphere's shape and size are also fluid. Changes in the solar wind, however, more strongly alter the fluctuating position of the boundaries on short timescales (hours to a few years). The solar wind's pressure varies far more rapidly than the outside pressure of the ISM at any given ...