Solar Wind
The solar wind is a stream of charged particles released from the upper atmosphere of the Sun, called the corona.
Description (Specifications)
This plasma consists of mostly electrons, protons and alpha particles with kinetic energy between 0.5 and 10 keV. Embedded within the solar-wind plasma is the interplanetary magnetic field. The solar wind varies in density, temperature and speed over time and over solar latitude and longitude. Its particles can escape the Sun's gravity because of their high energy resulting from the high temperature of the corona, which in turn is a result of the coronal magnetic field.
At a distance of more than a few solar radii from the Sun, the solar wind is supersonic and reaches speeds of 250 to 750 kilometers per second. The flow of the solar wind is no longer supersonic at the termination shock.
History & Background (Dossier)
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Image Repository
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References & Contributors (Sources)
This page uses content from Wikipedia. The original article was at wind Solar wind. The list of authors can be seen in the wind&action=history page history. The text of Wikipedia is available under the Commons Attribution-ShareAlike 3.0 Unported License. |
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- Author & Contributor: Lord (Marquis) and Master of Sophontology Maksim-Smelchak of the Ministry of Science