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QUIET-SUN INTENSITY CONTRASTS IN THE NEAR-ULTRAVIOLET AS MEASURED FROM SUNRISE
Hirzberger, J.,Feller, A.,Riethmü,ller, T. L.,Schü,ssler, M.,Borrero, J. M.,Afram, N.,Unruh, Y. C.,Berdyugina, S. V.,Gandorfer, A.,Solanki, S. K.,Barthol, P.,Bonet, J. A.,Martí,nez Pille IOP Publishing 2010 ASTROPHYSICAL JOURNAL LETTERS - Vol.723 No.2
Moving Magnetic Features Around a Pore
Kaithakkal, A. J.,Riethmü,ller, T. L.,Solanki, S. K.,Lagg, A.,Barthol, P.,Gandorfer, A.,Gizon, L.,Hirzberger, J.,vanNoort, M.,Rodrí,guez, J. Blanco,Iniesta, J. C. Del Toro,Suá,rez, D. American Astronomical Society 2017 The Astrophysical journal, Supplement series Vol.229 No.1
<P>Spectropolarimetric observations from SUNRISE/IMaX, obtained in 2013 June, are used for a statistical analysis to determine the physical properties of moving magnetic features (MMFs) observed near a pore. MMFs of the same and opposite polarity, with respect to the pore, are found to stream from its border at an average speed of 1.3 km s(-1) and 1.2 km s(-1), respectively, with mainly same-polarity MMFs found further away from the pore. MMFs of both polarities are found to harbor rather weak, inclined magnetic fields. Opposite-polarity MMFs are blueshifted, whereas same-polarity MMFs do not show any preference for up-or downflows. Most of the MMFs are found to be of sub-arcsecond size and carry a mean flux of similar to 1.2 x 10(17) Mx.</P>
COMPARISON BETWEEN Mg II<i>k</i>AND Ca II H IMAGES RECORDED BY SUNRISE/SuFI
Danilovic, S.,Hirzberger, J.,Riethmü,ller, T. L.,Solanki, S. K.,Barthol, P.,Berkefeld, T.,Gandorfer, A.,Gizon, L.,Knö,lker, M.,Schmidt, W.,Rodrí,guez, J. Blanco,Iniesta, J. C. Del Toro IOP Publishing 2014 The Astrophysical journal Vol.784 No.1
<P>We present a comparison of high-resolution images of the solar surface taken in the MgII k and Ca II H channels of the Filter Imager on the balloon-borne solar observatory SUNRISE. The Mg and Ca lines are sampled with 0.48 nm and 0.11 nm wide filters, respectively. The two channels show remarkable qualitative and quantitative similarities in the quiet Sun, in an active region plage and during a small flare. However, the Mg filtergrams display 1.4-1.7 times higher intensity contrast and appear more smeared and smoothed in the quiet Sun. In addition, the fibrils in a plage are wider. Although the exposure time is 100 times longer for Mg images, the evidence suggests that these differences cannot be explained only with instrumental effects or the evolution of the solar scene. The differences at least partially arise because of different line-formation heights, the stronger response of Mg k emission peaks to the higher temperatures, and the larger height range sampled by the broad Mg filter used here. This is evidently manifested during the flare when a surge in Mg evolves differently than in Ca.</P>
WAVES AS THE SOURCE OF APPARENT TWISTING MOTIONS IN SUNSPOT PENUMBRAE
Bharti, L.,Cameron, R. H.,Rempel, M.,Hirzberger, J.,Solanki, S. K. IOP Publishing 2012 The Astrophysical journal Vol.752 No.2
<P>The motion of dark striations across bright filaments in a sunspot penumbra has become an important new diagnostic of convective gas flows in penumbral filaments. The nature of these striations has, however, remained unclear. Here, we present an analysis of small-scale motions in penumbral filaments in both simulations and observations. The simulations, when viewed from above, show fine structure with dark lanes running outward from the dark core of the penumbral filaments. The dark lanes either occur preferentially on one side or alternate between both sides of the filament. We identify this fine structure with transverse (kink) oscillations of the filament, corresponding to a sideways swaying of the filament. These oscillations have periods in the range of 5-7 minutes and propagate outward and downward along the filament. Similar features are found in observed G-band intensity time series of penumbral filaments in a sunspot located near disk center obtained by the Broadband Filter Imager on board the Hinode. We also find that some filaments show dark striations moving to both sides of the filaments. Based on the agreement between simulations and observations we conclude that the motions of these striations are caused by transverse oscillations of the underlying bright filaments.</P>