The evolution of coronal magnetic fields

E. R. Priest; T. G. Forbes

doi:10.1007/BF00156802

The evolution of coronal magnetic fields

E. R. Priest^*, T. G. Forbes

^*Corresponding author for this work

Research output: Contribution to journal › Article › peer-review

Abstract

Slow photospheric motions can produce flow speeds in the corona which are fast enough to violate quasi-static evolution. Therefore, high-speed flows observed in the corona are not necessarily due to a loss of equilibrium or stability. In this letter we present an example where the flow speed increases indefinitely with, height, while the coronal magnetic energy increases quadratically with time.

Original language	English
Pages (from-to)	399-402
Number of pages	4
Journal	Solar Physics
Volume	130
Issue number	1-2
DOIs	https://doi.org/10.1007/BF00156802
Publication status	Published - Dec 1990

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title = "The evolution of coronal magnetic fields",

abstract = "Slow photospheric motions can produce flow speeds in the corona which are fast enough to violate quasi-static evolution. Therefore, high-speed flows observed in the corona are not necessarily due to a loss of equilibrium or stability. In this letter we present an example where the flow speed increases indefinitely with, height, while the coronal magnetic energy increases quadratically with time.",

author = "Priest, \{E. R.\} and Forbes, \{T. G.\}",

year = "1990",

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journal = "Solar Physics",

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T1 - The evolution of coronal magnetic fields

AU - Priest, E. R.

AU - Forbes, T. G.

PY - 1990/12

Y1 - 1990/12

N2 - Slow photospheric motions can produce flow speeds in the corona which are fast enough to violate quasi-static evolution. Therefore, high-speed flows observed in the corona are not necessarily due to a loss of equilibrium or stability. In this letter we present an example where the flow speed increases indefinitely with, height, while the coronal magnetic energy increases quadratically with time.

AB - Slow photospheric motions can produce flow speeds in the corona which are fast enough to violate quasi-static evolution. Therefore, high-speed flows observed in the corona are not necessarily due to a loss of equilibrium or stability. In this letter we present an example where the flow speed increases indefinitely with, height, while the coronal magnetic energy increases quadratically with time.

UR - https://www.scopus.com/pages/publications/0012443201

U2 - 10.1007/BF00156802

DO - 10.1007/BF00156802

M3 - Article

AN - SCOPUS:0012443201

SN - 0038-0938

VL - 130

SP - 399

EP - 402

JO - Solar Physics

JF - Solar Physics

IS - 1-2

ER -

The evolution of coronal magnetic fields

Abstract

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