Coronal hole: Difference between revisions
→Solar cycle: Removed incorrect info |
Shortened section names and added Template:Further |
||
| Line 3: | Line 3: | ||
A '''coronal hole''' is a temporary region of relatively cool, less dense [[plasma (physics)|plasma]] in the [[solar corona]] where the [[Sun]]'s [[magnetic field]] extends into [[interplanetary space]] as an open field.<ref name="Freedman, Roger A. 2008">Freedman, Roger A., and William J. Kaufmann III. "Our Star, the Sun." Universe. 8th ed. New York: W.H. Freeman, 2008. 419–420. Print.</ref> Compared to the corona's usual closed magnetic field that arches between regions of opposite magnetic polarity, the open magnetic field of a coronal hole allows [[solar wind]] to escape into space at a much quicker rate. This results in decreased temperature and density of the plasma at the site of a coronal hole as well as an increased speed in the average solar wind measured in interplanetary space.<ref name=r1>[http://www.ips.gov.au/Educational/2/1/5 What is a Coronal Hole?] ips.gov.au</ref> |
A '''coronal hole''' is a temporary region of relatively cool, less dense [[plasma (physics)|plasma]] in the [[solar corona]] where the [[Sun]]'s [[magnetic field]] extends into [[interplanetary space]] as an open field.<ref name="Freedman, Roger A. 2008">Freedman, Roger A., and William J. Kaufmann III. "Our Star, the Sun." Universe. 8th ed. New York: W.H. Freeman, 2008. 419–420. Print.</ref> Compared to the corona's usual closed magnetic field that arches between regions of opposite magnetic polarity, the open magnetic field of a coronal hole allows [[solar wind]] to escape into space at a much quicker rate. This results in decreased temperature and density of the plasma at the site of a coronal hole as well as an increased speed in the average solar wind measured in interplanetary space.<ref name=r1>[http://www.ips.gov.au/Educational/2/1/5 What is a Coronal Hole?] ips.gov.au</ref> |
||
==History== |
|||
==First discoveries== |
|||
In the 1960s, coronal holes showed up on X-ray images taken by [[sounding rockets]] and in observations at radio wavelengths by the [[Mills Cross Telescope|Sydney Chris Cross radio telescope]], but at the time it was unclear what they were. Their true nature was recognized in the 1970s when [[X-ray]] [[X-ray telescope|telescopes]] in the [[Skylab]] mission were flown above the Earth's atmosphere to reveal the structure of the corona.<ref name=r1/><ref name=r2>{{cite web|title=Massive Coronal Hole on the Sun|url=http://www.nasa.gov/mission_pages/sunearth/news/gallery/20130618-coronalhole.html|website=NASA|publisher=NASA|accessdate=31 October 2014}}</ref> |
In the 1960s, coronal holes showed up on X-ray images taken by [[sounding rockets]] and in observations at radio wavelengths by the [[Mills Cross Telescope|Sydney Chris Cross radio telescope]], but at the time it was unclear what they were. Their true nature was recognized in the 1970s when [[X-ray]] [[X-ray telescope|telescopes]] in the [[Skylab]] mission were flown above the Earth's atmosphere to reveal the structure of the corona.<ref name=r1/><ref name=r2>{{cite web|title=Massive Coronal Hole on the Sun|url=http://www.nasa.gov/mission_pages/sunearth/news/gallery/20130618-coronalhole.html|website=NASA|publisher=NASA|accessdate=31 October 2014}}</ref> |
||
==Solar cycle== |
==Solar cycle== |
||
{{Further|Solar cycle}} |
|||
[[File:Sun in X-Ray.png|thumb|A coronal hole at the Sun's north pole observed in [[soft X-ray]].]] |
[[File:Sun in X-Ray.png|thumb|A coronal hole at the Sun's north pole observed in [[soft X-ray]].]] |
||
Coronal hole size and population correspond with the [[solar cycle]]. As the Sun heads toward solar maximum the coronal holes move closer and closer to the Sun's poles.<ref name=r2/> During solar maximum, the number of coronal holes decreases until the magnetic fields on the Sun reverse. Afterwards new coronal holes appear near the new poles. The coronal holes then increase in size and number, extending farther from the poles as the Sun moves toward solar minimum again.<ref name=r3>{{cite web|last1=Fox|first1=Karen|title=Large Coronal Hole Near the Sun’s North Pole|url=http://www.nasa.gov/content/goddard/large-coronal-hole-near-sun-north-pole/|website=NASA|publisher=NASA|accessdate=31 October 2014}}</ref> |
Coronal hole size and population correspond with the [[solar cycle]]. As the Sun heads toward solar maximum the coronal holes move closer and closer to the Sun's poles.<ref name=r2/> During solar maximum, the number of coronal holes decreases until the magnetic fields on the Sun reverse. Afterwards new coronal holes appear near the new poles. The coronal holes then increase in size and number, extending farther from the poles as the Sun moves toward solar minimum again.<ref name=r3>{{cite web|last1=Fox|first1=Karen|title=Large Coronal Hole Near the Sun’s North Pole|url=http://www.nasa.gov/content/goddard/large-coronal-hole-near-sun-north-pole/|website=NASA|publisher=NASA|accessdate=31 October 2014}}</ref> |
||
== |
==Solar wind== |
||
{{Further|Solar wind}} |
|||
Coronal holes generally discharge [[solar wind]] at a speed about twice the average.<ref name=r2/> The escaping solar wind is known to travel along open magnetic field lines that pass through the coronal hole area.<ref name=r3/> Since coronal holes are regions in the Sun's corona that have much lower densities and temperatures than most of the corona, these regions are very thin. This thinness contributes to the solar wind since particles within the chromosphere can more easily break through. |
Coronal holes generally discharge [[solar wind]] at a speed about twice the average.<ref name=r2/> The escaping solar wind is known to travel along open magnetic field lines that pass through the coronal hole area.<ref name=r3/> Since coronal holes are regions in the Sun's corona that have much lower densities and temperatures than most of the corona, these regions are very thin. This thinness contributes to the solar wind since particles within the chromosphere can more easily break through. |
||
Revision as of 20:21, 25 January 2022
A coronal hole is a temporary region of relatively cool, less dense plasma in the solar corona where the Sun's magnetic field extends into interplanetary space as an open field.[1] Compared to the corona's usual closed magnetic field that arches between regions of opposite magnetic polarity, the open magnetic field of a coronal hole allows solar wind to escape into space at a much quicker rate. This results in decreased temperature and density of the plasma at the site of a coronal hole as well as an increased speed in the average solar wind measured in interplanetary space.[2]
History
In the 1960s, coronal holes showed up on X-ray images taken by sounding rockets and in observations at radio wavelengths by the Sydney Chris Cross radio telescope, but at the time it was unclear what they were. Their true nature was recognized in the 1970s when X-ray telescopes in the Skylab mission were flown above the Earth's atmosphere to reveal the structure of the corona.[2][3]
Solar cycle
Coronal hole size and population correspond with the solar cycle. As the Sun heads toward solar maximum the coronal holes move closer and closer to the Sun's poles.[3] During solar maximum, the number of coronal holes decreases until the magnetic fields on the Sun reverse. Afterwards new coronal holes appear near the new poles. The coronal holes then increase in size and number, extending farther from the poles as the Sun moves toward solar minimum again.[4]
Solar wind
Coronal holes generally discharge solar wind at a speed about twice the average.[3] The escaping solar wind is known to travel along open magnetic field lines that pass through the coronal hole area.[4] Since coronal holes are regions in the Sun's corona that have much lower densities and temperatures than most of the corona, these regions are very thin. This thinness contributes to the solar wind since particles within the chromosphere can more easily break through.
Influence on space weather
During solar minima coronal holes are the primary sources of space weather disturbances. Typically, geomagnetic (and proton) storms originating from coronal holes have a gradual commencement (over hours) and are not as severe as storms caused by coronal mass ejections (CMEs), which usually have a sudden onset. Due to the fact coronal holes can last for several months, it is often possible to predict the recurrence of this type of disturbance significantly farther in advance than for CME related disturbances.[2]
See also
References
- ^ Freedman, Roger A., and William J. Kaufmann III. "Our Star, the Sun." Universe. 8th ed. New York: W.H. Freeman, 2008. 419–420. Print.
- ^ a b c What is a Coronal Hole? ips.gov.au
- ^ a b c "Massive Coronal Hole on the Sun". NASA. NASA. Retrieved 31 October 2014.
- ^ a b Fox, Karen. "Large Coronal Hole Near the Sun's North Pole". NASA. NASA. Retrieved 31 October 2014.
Further reading
- Gombosi, Tamas (1998). Physics of the Space Environment. New York: Cambridge University Press. ISBN 0-521-59264-X.
- Jiang, Y., Chen, H., Shen, Y., Yang, L., & Li, K. (2007, January). Hα dimming associated with the eruption of a coronal sigmoid in the quiet Sun. Solar Physics, 240(1), 77–87.
