Solar magnetic elements at 0 Solar magnetic elements at 0.” 1 resolution General appearance and magnetic structure T.E. Berger etal. A&A 428,613,2004

1. Introduction 1)Motivation High temporal and space observation 2) Previous observations and theories ‘magnetic element hypothesis’ in active and quiet network regions discrete flux tubes ~100km ~kilogauss

1. Introduction 3)Main Results a) the magnetic structure with ~100km: ‘ribbon’ and discrete flux tubes b) two-component model: plage and enhanced network i) individual kilo-gauss flux tubes ii) ‘ribbon’ structure, from ~100 to ~1000 G

2. Observations 1) Telescope and instrumentation Swedish 1-m Solar Telescope (SST) ~0.”1 filter CaIIH G-band G-cont FeI  NiI  λ [nm] 369.88 430.5 436.4 630.25 676.78 ∆λwhm[nm] 0.29 1.1 1.1 0.0072 0.0086 Exposure time [ms] 35 5 5 200 120–144 Field of view [“] 82 × 83 82 × 83 82 × 83 98 × 66 98 × 66 Pixel size [“] 0.041 0.041 0.041 0.064 0.064 2) Observation program i) Selected the best images G-band, G-cont and CaIIH images 15s FeI magnetogram NiI Dopplergram 12s ii) Observed region the plage network of AR 10365 on 25 May 2003 , S7 E4 3) Example images

G-band

G-band continuum

CaII H -line

FeI magnetogram

NiI Dopplergram

3. Analysis Selected 6 regions of interest(ROI) 1)ROI 1 ‘ribbon-like’ structures 2)ROI 2 spread out ‘ribbon’ and ‘micropore’ 3)ROI 3 loop-like and ‘flower’ structures 4)ROI 4 two pores and canal structure 5)ROI 5 ‘ribbon’ and individual flux tubes brightest G, strongest FeI and NiI signals 6)ROI 6 ‘flower’, ribbon, pore, canal forming and individual flux tubes

G-band CaII H -line ROI 1 FeI magnetogram(-1177 to 478G) Binary mask of G-band

Intensity plot along the white line

G-band CaII H -line ROI 2 FeI magnetogram(-1438 to 242G) NiI Dopplergram(-783 to 878 ms-1)

Intensity plot along the white line

G-band CaII H -line ROI 3 FeI magnetogram (-1086 to 326G) NiI Dopplergram(-1531 to 785 ms-1)

G-band CaII H -line ROI 4 FeI magnetogram(-1438 to 502G) NiI Dopplergram(-453 to 970 ms-1)

572 ms-1 Intensity plot across the canal

G-band CaII H -line ROI 5 FeI magnetogram(-1055 to 435G) NiI Dopplergram(-1229 to 680 ms-1)

685ms-1 Intensity plot across the bright point

G-band CaII H -line ‘canal’ forming ‘flower’ ROI 6 FeI magnetogram(-1388 to 342 G) NiI Dopplergram(-958 to 1064 ms-1)

4. Conclusions 1)New finding: ‘ribbon-like’ structures 2)The magnetic structure with ~100km: ‘ribbon’ and discrete flux tubes 3) Propose two-component model: plage and enhanced network i) individual kilo-gauss flux tubes ~1500 G ii) ‘ribbon’ structure, from ~100 to ~1000 G 4) MHD simulation, dynamo flux generation, magnetic flux on convection … more complexity than previously thought