Editing Solar Wind
Jump to navigation
Jump to search
Warning: You are not logged in. Your IP address will be publicly visible if you make any edits. If you log in or create an account, your edits will be attributed to your username, along with other benefits.
The edit can be undone. Please check the comparison below to verify that this is what you want to do, and then save the changes below to finish undoing the edit.
| Latest revision | Your text | ||
| Line 1: | Line 1: | ||
[[File: Wiki Navy.png|right]] | [[File: Wiki Navy.png|right]] | ||
| − | The | + | The solar wind is a stream of charged particles released from the upper atmosphere of the Sun, called the corona. |
== Description ([[Specifications]]) == | == Description ([[Specifications]]) == | ||
| − | This plasma | + | 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 | + | 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. |
=== Image Repository === | === Image Repository === | ||
| Line 19: | Line 19: | ||
== References & Contributors ([[Sources]]) == | == References & Contributors ([[Sources]]) == | ||
| − | {{Wikipedia|Solar | + | {{Wikipedia|Solar wind}} |
{{Intermediate}} | {{Intermediate}} | ||
{{Detail}} | {{Detail}} | ||
| Line 29: | Line 29: | ||
| − | {{LEN| | + | {{LEN|}} |