Difference between revisions of "Solar wind"
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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). | 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). | ||
| − | + | ==Effect on Mars== | |
| + | It is believed that the solar wind is responsible for stripping around one third of Mars' [[atmosphere]] away and into space. Partly due to the Martian atmosphere's inability to retain its atmospheric gases due to the lack of a planetary [[magnetic field]] and the sheer voracity of the flow of ionizing solar wind particles, the solar wind is a major culprit for the [[atmosphere|low atmospheric pressure]] measured at the surface. | ||
==Counter Measures== | ==Counter Measures== | ||
Revision as of 13:14, 18 August 2011
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. The solar wind is often associated with Coronal Mass Ejections (CMEs), solar flares and coronal holes.
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. Like every other radioactive radiation it causes damage to material and health.
Contents
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).
Effect on Mars
It is believed that the solar wind is responsible for stripping around one third of Mars' atmosphere away and into space. Partly due to the Martian atmosphere's inability to retain its atmospheric gases due to the lack of a planetary magnetic field and the sheer voracity of the flow of ionizing solar wind particles, the solar wind is a major culprit for the low atmospheric pressure measured at the surface.
Counter Measures
Artificial magnetic field
The threat from solar wind can be managed through the generation of local magnetic fields. Recent research has shown that the size of the field need only be several hundred meters wide to provide protection to humans in space.[3] This magnetic shield could be scaled up to protect an entire settlement on the surface.
Shielding
While shielding a space ship increases its mass and fuel consumption, the shielding of a Martian colony is much easier, since the mass is only limited by structural stability constraints.
References
- ↑ "Solar Plasma Experiment" by Neugebauer & Snyder, Science, Volume 138, Issue 3545, pages 1095-1097, 1962
- ↑ "Origins of the Slow and the Ubiquitous Fast Solar Wind", Habbal et al., Astrophysical Journal Letters v.489, page L103, 1997
- ↑ The interaction of a flowing plasma with a dipole magnetic field: measurements and modelling of a diamagnetic cavity relevant to spacecraft protection. R Bamford et al 2008 Plasma Phys. Control. Fusion v.50, Issue124025 Pages 1-11
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