Coronal hole

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Coronal hole

Solar wind: ce MOS:RANGE

← Previous revision Revision as of 23:40, 18 April 2026
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Coronal holes are the primary source of fast [[solar wind]] streams, which escape more readily through their open magnetic field lines compared with the closed loops that confine plasma elsewhere in the corona.
Coronal holes are the primary source of fast [[solar wind]] streams, which escape more readily through their open magnetic field lines compared with the closed loops that confine plasma elsewhere in the corona.


[[Wave turbulence|Wave-driven turbulent]] heating and [[Alfvén wave|Alfvén-wave]] pressure accelerate plasma along the weakly diverging flux tubes rooted in coronal-hole interiors, producing 650-800 km/s flow speeds near 1 [[astronomical unit]] (AU).{{Citation |last1=Verdini |first1=Andrea |last2=Velli |first2=Marco |title=Turbulence-driven model for heating and acceleration of the fast wind in coronal holes |journal=The Astrophysical Journal Letters |volume=662 |pages=L111–L114 |year=2007 |doi=10.1086/519522 }}{{cite journal |last1=Cranmer |first1=Steven R. |last2=Gibson |first2=Sarah E. |last3=Riley |first3=Pete |title=Origins of the Ambient Solar Wind: Implications for Space Weather |journal=Space Science Reviews |date=November 2017 |volume=212 |issue=3–4 |pages=1345–1384 |doi=10.1007/s11214-017-0416-y |arxiv=1708.07169 |bibcode=2017SSRv..212.1345C }} The solar wind exists primarily in two alternating states referred to as the ''slow solar wind'' and the ''fast solar wind''. Fast streams originate inside coronal holes, whereas the slow component at 350-450 km/s often emerges from open-closed boundaries, active-region outflows, and pseudostreamer tops.{{Citation |last1=Brooks |first1=David H. |last2=Warren |first2=Harry P. |title=Connecting active-region outflows to the slow solar wind |journal=The Astrophysical Journal Letters |volume=727 |issue=1 |pages=L13 |year=2011 |doi=10.1088/2041-8205/727/1/L13 |arxiv=1009.4291 }}{{cite journal |last1=Geiss |first1=J. |last2=Gloeckler |first2=G. |last3=Von Steiger |first3=R. |title=Origin of the solar wind from composition data |journal=Space Science Reviews |date=April 1995 |volume=72 |issue=1–2 |pages=49–60 |doi=10.1007/BF00768753 |bibcode=1995SSRv...72...49G }}
[[Wave turbulence|Wave-driven turbulent]] heating and [[Alfvén wave|Alfvén-wave]] pressure accelerate plasma along the weakly diverging flux tubes rooted in coronal-hole interiors, producing 650–800 km/s flow speeds near 1 [[astronomical unit]] (AU).{{Citation |last1=Verdini |first1=Andrea |last2=Velli |first2=Marco |title=Turbulence-driven model for heating and acceleration of the fast wind in coronal holes |journal=The Astrophysical Journal Letters |volume=662 |pages=L111–L114 |year=2007 |doi=10.1086/519522 }}{{cite journal |last1=Cranmer |first1=Steven R. |last2=Gibson |first2=Sarah E. |last3=Riley |first3=Pete |title=Origins of the Ambient Solar Wind: Implications for Space Weather |journal=Space Science Reviews |date=November 2017 |volume=212 |issue=3–4 |pages=1345–1384 |doi=10.1007/s11214-017-0416-y |arxiv=1708.07169 |bibcode=2017SSRv..212.1345C }} The solar wind exists primarily in two alternating states referred to as the ''slow solar wind'' and the ''fast solar wind''. Fast streams originate inside coronal holes, whereas the slow component at 350–450 km/s often emerges from open-closed boundaries, active-region outflows, and pseudostreamer tops.{{Citation |last1=Brooks |first1=David H. |last2=Warren |first2=Harry P. |title=Connecting active-region outflows to the slow solar wind |journal=The Astrophysical Journal Letters |volume=727 |issue=1 |pages=L13 |year=2011 |doi=10.1088/2041-8205/727/1/L13 |arxiv=1009.4291 }}{{cite journal |last1=Geiss |first1=J. |last2=Gloeckler |first2=G. |last3=Von Steiger |first3=R. |title=Origin of the solar wind from composition data |journal=Space Science Reviews |date=April 1995 |volume=72 |issue=1–2 |pages=49–60 |doi=10.1007/BF00768753 |bibcode=1995SSRv...72...49G }}


Fast streams overtake slower wind ahead of them, creating stream interaction regions that corotate with the Sun and can steepen into forward and reverse shocks beyond 2 AU.{{Citation |last=Richardson |first=Ian G. |title=Solar wind stream interaction regions throughout the heliosphere |journal=Living Reviews in Solar Physics |volume=15 |issue=1 |article-number=1 |year=2018 |doi=10.1007/s41116-017-0011-z |pmid=30872980 |pmc=6390897 |bibcode=2018LRSP...15....1R }}{{cite journal |last1=Tsurutani |first1=Bruce T. |last2=Gonzalez |first2=Walter D. |last3=Gonzalez |first3=Alicia L. C. |last4=Guarnieri |first4=Fernando L. |last5=Gopalswamy |first5=Nat |last6=Grande |first6=Manuel |last7=Kamide |first7=Yohsuke |last8=Kasahara |first8=Yoshiya |last9=Lu |first9=Gang |last10=Mann |first10=Ian |last11=McPherron |first11=Robert |last12=Soraas |first12=Finn |last13=Vasyliunas |first13=Vytenis |title=Corotating solar wind streams and recurrent geomagnetic activity: A review |journal=Journal of Geophysical Research: Space Physics |date=July 2006 |volume=111 |issue=A7 |article-number=2005JA011273 |doi=10.1029/2005JA011273 |bibcode=2006JGRA..111.7S01T |url=http://urlib.net/sid.inpe.br/mtc-m16@80/2006/08.02.14.43 }}{{cite journal |last1=Temmer |first1=Manuela |title=Space weather: the solar perspective: An update to Schwenn (2006) |journal=Living Reviews in Solar Physics |date=December 2021 |volume=18 |issue=1 |page=4 |doi=10.1007/s41116-021-00030-3 |arxiv=2104.04261 |bibcode=2021LRSP...18....4T }}
Fast streams overtake slower wind ahead of them, creating stream interaction regions that corotate with the Sun and can steepen into forward and reverse shocks beyond 2 AU.{{Citation |last=Richardson |first=Ian G. |title=Solar wind stream interaction regions throughout the heliosphere |journal=Living Reviews in Solar Physics |volume=15 |issue=1 |article-number=1 |year=2018 |doi=10.1007/s41116-017-0011-z |pmid=30872980 |pmc=6390897 |bibcode=2018LRSP...15....1R }}{{cite journal |last1=Tsurutani |first1=Bruce T. |last2=Gonzalez |first2=Walter D. |last3=Gonzalez |first3=Alicia L. C. |last4=Guarnieri |first4=Fernando L. |last5=Gopalswamy |first5=Nat |last6=Grande |first6=Manuel |last7=Kamide |first7=Yohsuke |last8=Kasahara |first8=Yoshiya |last9=Lu |first9=Gang |last10=Mann |first10=Ian |last11=McPherron |first11=Robert |last12=Soraas |first12=Finn |last13=Vasyliunas |first13=Vytenis |title=Corotating solar wind streams and recurrent geomagnetic activity: A review |journal=Journal of Geophysical Research: Space Physics |date=July 2006 |volume=111 |issue=A7 |article-number=2005JA011273 |doi=10.1029/2005JA011273 |bibcode=2006JGRA..111.7S01T |url=http://urlib.net/sid.inpe.br/mtc-m16@80/2006/08.02.14.43 }}{{cite journal |last1=Temmer |first1=Manuela |title=Space weather: the solar perspective: An update to Schwenn (2006) |journal=Living Reviews in Solar Physics |date=December 2021 |volume=18 |issue=1 |page=4 |doi=10.1007/s41116-021-00030-3 |arxiv=2104.04261 |bibcode=2021LRSP...18....4T }}
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