Open AccessHigh‐speed solar‐wind streams and geospace interactions
Author(s) -
Kavanagh Andrew,
Denton Michael
Publication year - 2007
Publication title -
astronomy & geophysics
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 0.168
H-Index - 22
eISSN - 1468-4004
pISSN - 1366-8781
DOI - 10.1111/j.1468-4004.2007.48624.x
Subject(s) - solar wind , coronal mass ejection , coronal hole , physics , streams , nanoflares , magnetosphere , coronal cloud , coronal loop , corona (planetary geology) , helmet streamer , astronomy , environmental science , atmospheric sciences , plasma , astrobiology , computer science , computer network , quantum mechanics , venus
High-speed solar-wind streams emanate from solar coronal holes; the fast wind interacts with upstream slow streams producing regions of enhanced magnetic field strength and particle density that are known as co-rotating interaction regions. Due to the recurring nature of coronal holes near solar minimum, this results in periodic driving of the magnetosphere that can last for several days and input as much energy as a storm driven by a coronal mass ejection