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Träfflista för sökning "WFRF:(van Noort B) srt2:(2006-2009)"

Sökning: WFRF:(van Noort B) > (2006-2009)

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  • De Pontieu, B., et al. (författare)
  • Rapid Temporal Variability of Faculae: High-Resolution Observations and Modeling
  • 2006
  • Ingår i: The Astrophysical Journal. - : American Astronomical Society. - 0004-637X .- 1538-4357. ; 646:2, s. 1405-1420
  • Tidskriftsartikel (refereegranskat)abstract
    • We present high-resolution G-band observations (obtained with the Swedish 1 m Solar Telescope) of the rapid temporal variability of faculae, which occurs on granular timescales. By combining these observations with magnetoconvection simulations of a plage region, we show that much of this variability is not intrinsic to the magnetic field concentrations that are associated with faculae, but rather a phenomenon associated with the normal evolution and splitting of granules. We also show examples of facular variability caused by changes in the magnetic field, with movies of dynamic behavior of the striations that dominate much of the facular appearance at 0.1" resolution. Examples of these dynamics include merging, splitting, rapid motion, apparent fluting, and possibly swaying.
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  • Scharmer, Göran B., et al. (författare)
  • CRISP spectropolarimetric imaging of penumbral fine structure
  • 2008
  • Ingår i: Astrophysical Journal Letters. - : American Astronomical Society. - 2041-8205 .- 0004-637X .- 1538-4357. ; 689:1, s. L69-
  • Tidskriftsartikel (refereegranskat)abstract
    • We discuss penumbral fine structure in a small part of a pore, observed with the CRISP imaging spectropolarimeter at the Swedish 1-m Solar Telescope (SST), close to its diffraction limit of 0.16 . Milne-Eddington inversions applied to these Stokes data reveal large variations of field strength and inclination angle over dark-cored penumbral intrusions and a dark-cored light bridge. The mid-outer part of this penumbra structure shows 0.3 wide spines, separated by 1.6 (1200 km) and associated with 30° inclination variations. Between these spines, there are no small-scale magnetic structures that easily can be identified with individual flux tubes. A structure with nearly 10° more vertical and weaker magnetic field is seen midway between two spines. This structure is cospatial with the brightest penumbral filament, possibly indicating the location of a convective upflow from below.
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