Plasma flow versus magnetic feature-tracking speeds in the sun

G. Guerrero; M. Rheinhardt; A. Brandenburg; M. Dikpati

doi:10.1111/j.1745-3933.2011.01167.x

Plasma flow versus magnetic feature-tracking speeds in the sun

G. Guerrero, M. Rheinhardt, A. Brandenburg, M. Dikpati

Solar Frontiers

AlbaNova University Center

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

6 Scopus citations

Abstract

We simulate the magnetic feature-tracking (MFT) speed using axisymmetric advective- diffusive transport models in both one and two dimensions. By depositing magnetic bipolar regions at different latitudes at the Sun's surface and following their evolution for a prescribed meridional circulation and magnetic diffusivity profiles, we derive the MFT speed as a function of latitude. We find that in a one-dimensional surface-transport model the simulated MFT speed at the surface is always the same as the meridional flow speed used as input to the model, but is different in a two-dimensional transport model in the meridional (r, Θ) plane. The difference depends on the value of the magnetic diffusivity and on the radial gradient of the latitudinal velocity. We have confirmed our results with two different codes in spherical and Cartesian coordinates.

Original language	English
Pages (from-to)	L1-L5
Journal	Monthly Notices of the Royal Astronomical Society: Letters
Volume	420
Issue number	1
DOIs	https://doi.org/10.1111/j.1745-3933.2011.01167.x
State	Published - Feb 2012

Keywords

Convection
MHD
Magnetic fields
Sun: activity
Surface magnetism

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10.1111/j.1745-3933.2011.01167.x

Cite this

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title = "Plasma flow versus magnetic feature-tracking speeds in the sun",

abstract = "We simulate the magnetic feature-tracking (MFT) speed using axisymmetric advective- diffusive transport models in both one and two dimensions. By depositing magnetic bipolar regions at different latitudes at the Sun's surface and following their evolution for a prescribed meridional circulation and magnetic diffusivity profiles, we derive the MFT speed as a function of latitude. We find that in a one-dimensional surface-transport model the simulated MFT speed at the surface is always the same as the meridional flow speed used as input to the model, but is different in a two-dimensional transport model in the meridional (r, Θ) plane. The difference depends on the value of the magnetic diffusivity and on the radial gradient of the latitudinal velocity. We have confirmed our results with two different codes in spherical and Cartesian coordinates.",

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T1 - Plasma flow versus magnetic feature-tracking speeds in the sun

AU - Guerrero, G.

AU - Rheinhardt, M.

AU - Brandenburg, A.

AU - Dikpati, M.

PY - 2012/2

Y1 - 2012/2

N2 - We simulate the magnetic feature-tracking (MFT) speed using axisymmetric advective- diffusive transport models in both one and two dimensions. By depositing magnetic bipolar regions at different latitudes at the Sun's surface and following their evolution for a prescribed meridional circulation and magnetic diffusivity profiles, we derive the MFT speed as a function of latitude. We find that in a one-dimensional surface-transport model the simulated MFT speed at the surface is always the same as the meridional flow speed used as input to the model, but is different in a two-dimensional transport model in the meridional (r, Θ) plane. The difference depends on the value of the magnetic diffusivity and on the radial gradient of the latitudinal velocity. We have confirmed our results with two different codes in spherical and Cartesian coordinates.

AB - We simulate the magnetic feature-tracking (MFT) speed using axisymmetric advective- diffusive transport models in both one and two dimensions. By depositing magnetic bipolar regions at different latitudes at the Sun's surface and following their evolution for a prescribed meridional circulation and magnetic diffusivity profiles, we derive the MFT speed as a function of latitude. We find that in a one-dimensional surface-transport model the simulated MFT speed at the surface is always the same as the meridional flow speed used as input to the model, but is different in a two-dimensional transport model in the meridional (r, Θ) plane. The difference depends on the value of the magnetic diffusivity and on the radial gradient of the latitudinal velocity. We have confirmed our results with two different codes in spherical and Cartesian coordinates.

KW - Convection

KW - MHD

KW - Magnetic fields

KW - Sun: activity

KW - Surface magnetism

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DO - 10.1111/j.1745-3933.2011.01167.x

M3 - Article

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JO - Monthly Notices of the Royal Astronomical Society: Letters

JF - Monthly Notices of the Royal Astronomical Society: Letters

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Plasma flow versus magnetic feature-tracking speeds in the sun

Abstract

Keywords

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