1. 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

2. 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

3. 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

4. 2. Observations 1) Telescope and instrumentation
Swedish 1-m Solar Telescope (SST) ~0.”1
filter CaIIH G-band G-cont FeI  NiI 
λ [nm]
∆λwhm[nm]
Exposure time [ms] –144
Field of view [“] 82 × × × × × 66
Pixel size [“]
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 on 25 May 2003 , S7 E4
3) Example images

5. G-band

6. G-band continuum

7. CaII H -line

8. FeI magnetogram

9. NiI Dopplergram

10. 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

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

12. Intensity plot along the white line

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

14. Intensity plot along the white line

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

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

17. 572 ms-1
Intensity plot across the canal

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

19. 685ms-1
Intensity plot across the bright point

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

21. 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