Kinematics of Magnetic Bright Features in the Solar Photosphere

DOI: 
10.3847/1538-4365/229/1/8
Publication date: 
17/04/2017
Main author: 
Jafarzadeh S.
IAA authors: 
Iniesta, J.C.D.T.;Suárez, D.O.
Authors: 
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.
Journal: 
Astrophysical Journal, Supplement Series
Refereed: 
Yes
Publication type: 
Article
Volume: 
229
Number: 
8
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%. © 2017. The American Astronomical Society. All rights reserved..

Database: 
SCOPUS
ADS
URL: 
https://www.scopus.com/inward/record.uri?eid=2-s2.0-85016430873&doi=10.3847%2f1538-4365%2f229%2f1%2f8&partnerID=40&md5=e65a66c4f79d9609dd252ef46b1e7835
ADS Bibcode: 
2017ApJS..229....8J
Keywords: 
methods: observational; Sun: magnetic fields; Sun: photosphere