Resistive ballooning modes in line-tied coronal fields. II - Loops

M. Velli; A. W. Hood

doi:10.1007/BF00160657

Resistive ballooning modes in line-tied coronal fields. II - Loops

M. Velli, A. W. Hood

Applied Mathematics

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

Abstract

The resistive stability of coronal loops to perturbations with short wavelength across the magnetic field is analysed, taking full account of the line tying effect due to the presence of the photosphere. The results presented are similar to those previously obtained for arcades: configurations with a pressure profile decreasing with distance from the loop axis at some point are found to be always unstable, the growth rate γ increasing monotonically with the wavenumber (n) and scaling approximately as γ ≡ (n2Dr)1/3 in the limit of large n.

Original language	English
Pages (from-to)	351-354
Journal	Solar Physics
Volume	109
DOIs	https://doi.org/10.1007/BF00160657
Publication status	Published - 1 Sept 1987

Keywords

Coronal Loops
Perturbation Theory
Plasma Density
Solar Corona
Solar Magnetic Field
Differential Equations
Equilibrium Equations
Numerical Analysis

Access to Document

10.1007/BF00160657

http://adsabs.harvard.edu/abs/1987SoPh..109..351V

Cite this

@article{ba78637f4aae4d848adee72e1d2c14c3,

title = "Resistive ballooning modes in line-tied coronal fields. II - Loops",

abstract = "The resistive stability of coronal loops to perturbations with short wavelength across the magnetic field is analysed, taking full account of the line tying effect due to the presence of the photosphere. The results presented are similar to those previously obtained for arcades: configurations with a pressure profile decreasing with distance from the loop axis at some point are found to be always unstable, the growth rate γ increasing monotonically with the wavenumber (n) and scaling approximately as γ ≡ (n2Dr)1/3 in the limit of large n.",

keywords = "Coronal Loops, Perturbation Theory, Plasma Density, Solar Corona, Solar Magnetic Field, Differential Equations, Equilibrium Equations, Numerical Analysis",

author = "M. Velli and Hood, {A. W.}",

year = "1987",

month = sep,

day = "1",

doi = "10.1007/BF00160657",

language = "English",

volume = "109",

pages = "351--354",

journal = "Solar Physics",

issn = "0038-0938",

publisher = "Springer",

}

TY - JOUR

T1 - Resistive ballooning modes in line-tied coronal fields. II - Loops

AU - Velli, M.

AU - Hood, A. W.

PY - 1987/9/1

Y1 - 1987/9/1

N2 - The resistive stability of coronal loops to perturbations with short wavelength across the magnetic field is analysed, taking full account of the line tying effect due to the presence of the photosphere. The results presented are similar to those previously obtained for arcades: configurations with a pressure profile decreasing with distance from the loop axis at some point are found to be always unstable, the growth rate γ increasing monotonically with the wavenumber (n) and scaling approximately as γ ≡ (n2Dr)1/3 in the limit of large n.

AB - The resistive stability of coronal loops to perturbations with short wavelength across the magnetic field is analysed, taking full account of the line tying effect due to the presence of the photosphere. The results presented are similar to those previously obtained for arcades: configurations with a pressure profile decreasing with distance from the loop axis at some point are found to be always unstable, the growth rate γ increasing monotonically with the wavenumber (n) and scaling approximately as γ ≡ (n2Dr)1/3 in the limit of large n.

KW - Coronal Loops

KW - Perturbation Theory

KW - Plasma Density

KW - Solar Corona

KW - Solar Magnetic Field

KW - Differential Equations

KW - Equilibrium Equations

KW - Numerical Analysis

U2 - 10.1007/BF00160657

DO - 10.1007/BF00160657

M3 - Article

SN - 0038-0938

VL - 109

SP - 351

EP - 354

JO - Solar Physics

JF - Solar Physics

ER -

Resistive ballooning modes in line-tied coronal fields. II - Loops

Abstract

Keywords

Access to Document

Fingerprint

Cite this