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The magnetic properties of photospheric magnetic bright points with high resolution spectropolarimetry
journal contribution
posted on 2019-09-01, 00:00 authored by Peter H Keys, Aaron Reid, Mihalis Mathioudakis, Sergiy ShelyagSergiy Shelyag, Vasco M J Henriques, Rebecca L Hewitt, Dario Del Moro, Shahin Jafarzadeh, David B Jess, Marco StangaliniMagnetic bright points are small-scale magnetic elements ubiquitous across the solar disk, with the prevailing theory suggesting that they form due to the process of convective collapse. Employing a unique full Stokes spectropolarimetric data set of a quiet Sun region close to disk centre obtained with the Swedish Solar Telescope, we look at general trends in the properties of magnetic bright points. In total we track 300 MBPs in the data set and we employ NICOLE inversions to ascertain various parameters for the bright points such as line-of-sight magnetic field strength and line-of-sight velocity, for comparison. We observe a bimodal distribution in terms of maximum magnetic field strength in the bright points with peaks at ∼480 G and ∼1700 G, although we cannot attribute the kilogauss fields in this distribution solely to the process of convective collapse. Analysis of MURaM simulations does not return the same bimodal distribution. However, the simulations provide strong evidence that the emergence of new flux and diffusion of this new flux play a significant role in generating the weak bright point distribution seen in our observations.
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Journal
Monthly notices of the Royal Astronomical Society: lettersVolume
488Issue
1Pagination
1 - 6Publisher
Oxford University PressLocation
Oxford, Eng.Publisher DOI
ISSN
1745-3925eISSN
1745-3933Language
engPublication classification
C1 Refereed article in a scholarly journalCopyright notice
2019, The Author(s)Usage metrics
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