Kinematics of Magnetic Bright Features in the Solar Photosphere

S. Jafarzadeh; S. K. Solanki; R. H. Cameron; P. Barthol; J. Blanco Rodríguez; J. C.Del Toro Iniesta; A. Gandorfer; L. Gizon; J. Hirzberger; M. Knölker; V. Martínez Pillet; D. Orozco Suárez; T. L. Riethmüller; W. Schmidt; M. Van Noort

doi:10.3847/1538-4365/229/1/8

Kinematics of Magnetic Bright Features in the Solar Photosphere

S. Jafarzadeh, S. K. Solanki, R. H. Cameron, P. Barthol, J. Blanco Rodríguez, J. C.Del Toro Iniesta, A. Gandorfer, L. Gizon, J. Hirzberger, M. Knölker, V. Martínez Pillet, D. Orozco Suárez, T. L. Riethmüller, W. Schmidt, M. Van Noort

Center for Space Science

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Abstract

Convective flows are known as the prime means of transporting magnetic fields on the solar surface. Thus, small magnetic structures are good tracers of turbulent flows. We study the migration and dispersal of magnetic bright features (MBFs) in intergranular areas observed at high spatial resolution with Sunrise/IMaX. We describe the flux dispersal of individual MBFs as a diffusion process whose parameters are computed for various areas in the quiet-Sun and the vicinity of active regions from seeing-free data. We find that magnetic concentrations are best described as random walkers close to network areas (diffusion index, γ = 1.0), travelers with constant speeds over a supergranule (γ = 1.9-2.0), and decelerating movers in the vicinity of flux emergence and/or within active regions (γ 1.4-1.5). The three types of regions host MBFs with mean diffusion coefficients of 130 km² s^-1, 80-90 km² s^-1, and 25-70 km² s^-1, respectively. The MBFs in these three types of regions are found to display a distinct kinematic behavior at a confidence level in excess of 95%.

Original language	English (US)
Article number	8
Journal	Astrophysical Journal, Supplement Series
Volume	229
Issue number	1
DOIs	https://doi.org/10.3847/1538-4365/229/1/8
State	Published - Mar 2017

Keywords

Sun: magnetic fields
Sun: photosphere
methods: observational

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.3847/1538-4365/229/1/8

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Jafarzadeh, S., Solanki, S. K., Cameron, R. H., Barthol, P., Rodríguez, J. B., Iniesta, J. C. D. T., Gandorfer, A., Gizon, L., Hirzberger, J., Knölker, M., Pillet, V. M., Suárez, D. O., Riethmüller, T. L., Schmidt, W., & Noort, M. V. (2017). Kinematics of Magnetic Bright Features in the Solar Photosphere. Astrophysical Journal, Supplement Series, 229(1), Article 8. https://doi.org/10.3847/1538-4365/229/1/8

Jafarzadeh, S, Solanki, SK, Cameron, RH, Barthol, P, Rodríguez, JB, Iniesta, JCDT, Gandorfer, A, Gizon, L, Hirzberger, J, Knölker, M, Pillet, VM, Suárez, DO, Riethmüller, TL, Schmidt, W & Noort, MV 2017, 'Kinematics of Magnetic Bright Features in the Solar Photosphere', Astrophysical Journal, Supplement Series, vol. 229, no. 1, 8. https://doi.org/10.3847/1538-4365/229/1/8

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abstract = "Convective flows are known as the prime means of transporting magnetic fields on the solar surface. Thus, small magnetic structures are good tracers of turbulent flows. We study the migration and dispersal of magnetic bright features (MBFs) in intergranular areas observed at high spatial resolution with Sunrise/IMaX. We describe the flux dispersal of individual MBFs as a diffusion process whose parameters are computed for various areas in the quiet-Sun and the vicinity of active regions from seeing-free data. We find that magnetic concentrations are best described as random walkers close to network areas (diffusion index, γ = 1.0), travelers with constant speeds over a supergranule (γ = 1.9-2.0), and decelerating movers in the vicinity of flux emergence and/or within active regions (γ 1.4-1.5). The three types of regions host MBFs with mean diffusion coefficients of 130 km2 s-1, 80-90 km2 s-1, and 25-70 km2 s-1, respectively. The MBFs in these three types of regions are found to display a distinct kinematic behavior at a confidence level in excess of 95%.",

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AU - Jafarzadeh, S.

AU - Solanki, S. K.

AU - Cameron, R. H.

AU - Barthol, P.

AU - Rodríguez, J. Blanco

AU - Iniesta, J. C.Del Toro

AU - Gandorfer, A.

AU - Gizon, L.

AU - Hirzberger, J.

AU - Knölker, M.

AU - Pillet, V. Martínez

AU - Suárez, D. Orozco

AU - Riethmüller, T. L.

AU - Schmidt, W.

AU - Noort, M. Van

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N2 - Convective flows are known as the prime means of transporting magnetic fields on the solar surface. Thus, small magnetic structures are good tracers of turbulent flows. We study the migration and dispersal of magnetic bright features (MBFs) in intergranular areas observed at high spatial resolution with Sunrise/IMaX. We describe the flux dispersal of individual MBFs as a diffusion process whose parameters are computed for various areas in the quiet-Sun and the vicinity of active regions from seeing-free data. We find that magnetic concentrations are best described as random walkers close to network areas (diffusion index, γ = 1.0), travelers with constant speeds over a supergranule (γ = 1.9-2.0), and decelerating movers in the vicinity of flux emergence and/or within active regions (γ 1.4-1.5). The three types of regions host MBFs with mean diffusion coefficients of 130 km2 s-1, 80-90 km2 s-1, and 25-70 km2 s-1, respectively. The MBFs in these three types of regions are found to display a distinct kinematic behavior at a confidence level in excess of 95%.

AB - Convective flows are known as the prime means of transporting magnetic fields on the solar surface. Thus, small magnetic structures are good tracers of turbulent flows. We study the migration and dispersal of magnetic bright features (MBFs) in intergranular areas observed at high spatial resolution with Sunrise/IMaX. We describe the flux dispersal of individual MBFs as a diffusion process whose parameters are computed for various areas in the quiet-Sun and the vicinity of active regions from seeing-free data. We find that magnetic concentrations are best described as random walkers close to network areas (diffusion index, γ = 1.0), travelers with constant speeds over a supergranule (γ = 1.9-2.0), and decelerating movers in the vicinity of flux emergence and/or within active regions (γ 1.4-1.5). The three types of regions host MBFs with mean diffusion coefficients of 130 km2 s-1, 80-90 km2 s-1, and 25-70 km2 s-1, respectively. The MBFs in these three types of regions are found to display a distinct kinematic behavior at a confidence level in excess of 95%.

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KW - Sun: photosphere

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Kinematics of Magnetic Bright Features in the Solar Photosphere

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Keywords

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