Influence of non-potential coronal magnetic topology on solar wind models

Sarah Jane Edwards; Anthony Robinson Yeates; Francois Bocquet; Duncan Hendry Mackay

doi:10.1007/s11207-015-0795-8

Influence of non-potential coronal magnetic topology on solar wind models

Sarah Jane Edwards, Anthony Robinson Yeates, Francois Bocquet, Duncan Hendry Mackay

Applied Mathematics

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

Abstract

By comparing a magneto-frictional model of the low coronal magnetic field to
a potential field source surface model, we investigate the possible impact of non-potential magnetic structure on empirical solar wind models. These empirical models (such as Wang-Sheeley-Arge) estimate the distribution of solar wind speed solely from the magnetic field structure in the low corona. Our models are computed in a domain between the solar surface and 2.5 solar radii, and are extended to 0.1 AU using a Schatten current sheet model. The non-potential field has a more complex magnetic skeleton and quasi-separatrix structures than the potential field, leading to different sub-structure in the solar wind speed proxies. It contains twisted magnetic structures which can perturb the separatrix surfaces traced down from the base of the heliospheric current sheet. A significant difference between the models is the greater amount of open magnetic flux in the non-potential model. Using existing empirical formulae this leads to higher predicted wind speeds for two reasons: partly because magnetic
flux tubes expand less rapidly with height, but more importantly because more open field lines are further from coronal hole boundaries.

Original language	English
Pages (from-to)	2791-2808
Number of pages	18
Journal	Solar Physics
Volume	290
Issue number	10
Early online date	28 Oct 2015
DOIs	https://doi.org/10.1007/s11207-015-0795-8
Publication status	Published - Oct 2015

Keywords

Corona, models
Magnetic fields, corona
Magnetic fields, interplanetary
Magnetic fields, models
Solar wind, theory

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10.1007/s11207-015-0795-8

1511.00427v1
© 2015, Publisher / the Author(s). This work is made available online in accordance with the publisher’s policies. This is the author created, accepted version manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at link.springer.com / https://dx.doi.org/10.1007/s11207-015-0795-8
Accepted author manuscript, 1.73 MB

Cite this

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title = "Influence of non-potential coronal magnetic topology on solar wind models",

abstract = "By comparing a magneto-frictional model of the low coronal magnetic field toa potential field source surface model, we investigate the possible impact of non-potential magnetic structure on empirical solar wind models. These empirical models (such as Wang-Sheeley-Arge) estimate the distribution of solar wind speed solely from the magnetic field structure in the low corona. Our models are computed in a domain between the solar surface and 2.5 solar radii, and are extended to 0.1 AU using a Schatten current sheet model. The non-potential field has a more complex magnetic skeleton and quasi-separatrix structures than the potential field, leading to different sub-structure in the solar wind speed proxies. It contains twisted magnetic structures which can perturb the separatrix surfaces traced down from the base of the heliospheric current sheet. A significant difference between the models is the greater amount of open magnetic flux in the non-potential model. Using existing empirical formulae this leads to higher predicted wind speeds for two reasons: partly because magnetic flux tubes expand less rapidly with height, but more importantly because more open field lines are further from coronal hole boundaries.",

keywords = "Corona, models, Magnetic fields, corona, Magnetic fields, interplanetary, Magnetic fields, models, Solar wind, theory",

author = "Edwards, {Sarah Jane} and Yeates, {Anthony Robinson} and Francois Bocquet and Mackay, {Duncan Hendry}",

year = "2015",

month = oct,

doi = "10.1007/s11207-015-0795-8",

language = "English",

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journal = "Solar Physics",

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AU - Edwards, Sarah Jane

AU - Yeates, Anthony Robinson

AU - Bocquet, Francois

AU - Mackay, Duncan Hendry

PY - 2015/10

Y1 - 2015/10

N2 - By comparing a magneto-frictional model of the low coronal magnetic field toa potential field source surface model, we investigate the possible impact of non-potential magnetic structure on empirical solar wind models. These empirical models (such as Wang-Sheeley-Arge) estimate the distribution of solar wind speed solely from the magnetic field structure in the low corona. Our models are computed in a domain between the solar surface and 2.5 solar radii, and are extended to 0.1 AU using a Schatten current sheet model. The non-potential field has a more complex magnetic skeleton and quasi-separatrix structures than the potential field, leading to different sub-structure in the solar wind speed proxies. It contains twisted magnetic structures which can perturb the separatrix surfaces traced down from the base of the heliospheric current sheet. A significant difference between the models is the greater amount of open magnetic flux in the non-potential model. Using existing empirical formulae this leads to higher predicted wind speeds for two reasons: partly because magnetic flux tubes expand less rapidly with height, but more importantly because more open field lines are further from coronal hole boundaries.

AB - By comparing a magneto-frictional model of the low coronal magnetic field toa potential field source surface model, we investigate the possible impact of non-potential magnetic structure on empirical solar wind models. These empirical models (such as Wang-Sheeley-Arge) estimate the distribution of solar wind speed solely from the magnetic field structure in the low corona. Our models are computed in a domain between the solar surface and 2.5 solar radii, and are extended to 0.1 AU using a Schatten current sheet model. The non-potential field has a more complex magnetic skeleton and quasi-separatrix structures than the potential field, leading to different sub-structure in the solar wind speed proxies. It contains twisted magnetic structures which can perturb the separatrix surfaces traced down from the base of the heliospheric current sheet. A significant difference between the models is the greater amount of open magnetic flux in the non-potential model. Using existing empirical formulae this leads to higher predicted wind speeds for two reasons: partly because magnetic flux tubes expand less rapidly with height, but more importantly because more open field lines are further from coronal hole boundaries.

KW - Corona, models

KW - Magnetic fields, corona

KW - Magnetic fields, interplanetary

KW - Magnetic fields, models

KW - Solar wind, theory

UR - http://link.springer.com/article/10.1007/s11207-015-0795-8

U2 - 10.1007/s11207-015-0795-8

DO - 10.1007/s11207-015-0795-8

M3 - Article

SN - 0038-0938

VL - 290

SP - 2791

EP - 2808

JO - Solar Physics

JF - Solar Physics

IS - 10

ER -

Influence of non-potential coronal magnetic topology on solar wind models

Abstract

Keywords

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Space Weather Prediction for Met Office: Space Weather Prediction for Met Office

Plasma Theory: Solar and Magnetospheric Plasma Theory

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Influence of non-potential coronal magnetic topology on solar wind models

Abstract

Keywords

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Projects

Space Weather Prediction for Met Office: Space Weather Prediction for Met Office

Plasma Theory: Solar and Magnetospheric Plasma Theory

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