Difference between revisions of "Solar wind"
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The '''solar wind''' is the continuous stream of energetic and ionized particles from the [[Sun]] that extends far into interplanetary space following the interplanetary magnetic field (IMF). The ''solar wind'' strongly interacts with magnetic fields of the planets and will often manifest itself as [[aurora|aurorae]] in the upper atmospheres of planets with magnetic fields. In the case of Mars, with a weak (often considered to be non-existent) global magnetic field, solar wind particles have greater penetration into the atmosphere creating a hazard to any future [[hill-side concept|human settlements]] on the surface. The ''solar wind'' is often associated with [[Coronal Mass Ejections]] (CMEs), [[solar flares]] and coronal holes. | The '''solar wind''' is the continuous stream of energetic and ionized particles from the [[Sun]] that extends far into interplanetary space following the interplanetary magnetic field (IMF). The ''solar wind'' strongly interacts with magnetic fields of the planets and will often manifest itself as [[aurora|aurorae]] in the upper atmospheres of planets with magnetic fields. In the case of Mars, with a weak (often considered to be non-existent) global magnetic field, solar wind particles have greater penetration into the atmosphere creating a hazard to any future [[hill-side concept|human settlements]] on the surface. The ''solar wind'' is often associated with [[Coronal Mass Ejections]] (CMEs), [[solar flares]] and coronal holes. | ||
| − | {{SettlementIndex}} | + | ==Characteristics== |
| + | The solar wind is characterised as a constant flow of plasma from the chromosphere into interplanetary space. Understood to be ''bi-modal'', the solar wind consists of two distinct streams. The ''fast'' solar wind travels at velocities of between 700-900 km/s<ref>[http://adsabs.harvard.edu/abs/1962Sci...138.1095N "''Solar Plasma Experiment''" by Neugebauer & Snyder, ''Science'', Volume 138, Issue 3545, pages 1095-1097, '''1962''']</ref> and is associated with open magnetic flux (i.e. coronal holes located in solar polar regions). The ''slow'' solar wind travels at velocities of between 300-400 km/s<ref>[http://adsabs.harvard.edu/abs/1997ApJ...489L.103H "''Origins of the Slow and the Ubiquitous Fast Solar Wind''", Habbal ''et al.'', ''Astrophysical Journal Letters'' v.489, page L103, '''1997''']</ref> and is located above equatorial closed magnetic flux regions (i.e. the streamer belt). | ||
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| + | ===References=== | ||
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[[Category:Space Weather]] | [[Category:Space Weather]] | ||
Revision as of 00:18, 17 December 2007
The solar wind is the continuous stream of energetic and ionized particles from the Sun that extends far into interplanetary space following the interplanetary magnetic field (IMF). The solar wind strongly interacts with magnetic fields of the planets and will often manifest itself as aurorae in the upper atmospheres of planets with magnetic fields. In the case of Mars, with a weak (often considered to be non-existent) global magnetic field, solar wind particles have greater penetration into the atmosphere creating a hazard to any future human settlements on the surface. The solar wind is often associated with Coronal Mass Ejections (CMEs), solar flares and coronal holes.
Characteristics
The solar wind is characterised as a constant flow of plasma from the chromosphere into interplanetary space. Understood to be bi-modal, the solar wind consists of two distinct streams. The fast solar wind travels at velocities of between 700-900 km/s[1] and is associated with open magnetic flux (i.e. coronal holes located in solar polar regions). The slow solar wind travels at velocities of between 300-400 km/s[2] and is located above equatorial closed magnetic flux regions (i.e. the streamer belt).
References
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