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Reconstruction of solar magnetic field since 1700 onwards

工作汇报（ 2 ）. Reconstruction of solar magnetic field since 1700 onwards. 姜 杰. In collaboration with Robert Cameron, Dieter Schmitt and Manfred Schuessler. Free parameter. Complements of Talk 1. Initial condition. e-folding time of approximately 4000 years. Decay time:.

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Reconstruction of solar magnetic field since 1700 onwards

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  1. 工作汇报（2） Reconstruction of solar magnetic field since 1700 onwards 姜 杰 In collaboration with Robert Cameron, Dieter Schmitt and Manfred Schuessler 工作汇报(2)

  2. Free parameter Complements of Talk 1 Initial condition e-folding time of approximately 4000 years 工作汇报(2)

  3. Decay time: Complements of Talk 1 The way to deal with radial diffusion 工作汇报(2)

  4. Towards 300 yrs recon. – Modeling cys. 15-21 Old result • Locations and areas of sunspots groups: Royal Greenwich Observatory (1874 -- 1976) USAF/NOAA (1976 onwards) Sunspot Data • Tilt angles of sunspots groups: Mount Wilson (1917 -- 1985) Kodaikanal (1906 -- 1987) 工作汇报(2)

  5. Cycle variation of sunspot group tilts 工作汇报(2)

  6. Modeling cys. 15-21: results * Makarov et al. (2003) simulation aa-index (Lockwood) 工作汇报(2)

  7. Modeling cys. 15-21: results 极区磁场和前一活动周的强度没有相关性， 而和其下一活动周的强度有很好的相关性 工作汇报(2)

  8. l = 1; m = 0 l = 1; m = 1 ～ About open flux Low order modes Axial dipole field Equatorial dipole field axi. dip. (solar mini.) Lati. sep. Open flux equ. dip. (solar maxi.) Long. sep. 工作汇报(2)

  9. How can we go back further ? 工作汇报(2)

  10. Characteristics of sunspot group emergence Sunspot number Sunspot number datasets 工作汇报(2)

  11. Datasets (1874 — 1976, cy. 12-20): • Sunspot groups (RGO) • sunspot number (RG) • Statistical properties of sunspot group emergence (latitude, longitude, area and tilt angle) as functions of the cycle strength and of time during the solar cycle defined by sunspot number. 工作汇报(2)

  12. Latitude distribution 工作汇报(2)

  13. Mean lati. vs. cycle strength 工作汇报(2)

  14. A comparison of the mean lati. for cycles 12--20 工作汇报(2)

  15. Width of the lati. distribution 工作汇报(2)

  16. Longitude distribution Eq. dipole (moment) of a sunspot group ( ) in direction in N. Hem. Eq. dipole of all the SGs from both Hem.emerging between times t and The magnitude of the observed sunspot dipole (moment) 工作汇报(2)

  17. The difference between reflects the amount of nesting Longitude distribution 工作汇报(2)

  18. Area distribution Area distribution function 工作汇报(2)

  19. Cycle phase dependence of area distribution 工作汇报(2)

  20. Tilt angle distribution 工作汇报(2)

  21. Number of sunspot groups as a function of time 工作汇报(2)

  22. Reconstruction of butterfly diagram (1) Obs. Sim. 工作汇报(2)

  23. Reconstruction of butterfly diagram (2) 工作汇报(2)

  24. Reconstruction of butterfly diagram (3) 工作汇报(2)

  25. Flow chart Input: sunspot number dataset lati., area & tilt angle random longitudes (lowest eq. DM) lati., area & tilt angle 2 active longitudes (highest eq. DM) SFT (20 runs) SFT (20 runs) solar surface field (1) solar surface field (2) CSSS extrapolation Zhao & Hoeksema (1995) Polar field (1)=(2) 20 runs average CSSS extrapolation Zhao & Hoeksema (1995) source surface field source surface field 1- c% c% Open field20 runs average 工作汇报(2)

  26. Calibration of the parameter of active long. 工作汇报(2)

  27. The case without radial diffusion CJSS10 工作汇报(2)

  28. The case with weak radial diffusion Less reliable sunspot number rms diff. 14%  20% Polar field vs. solar cycle becomes weak 工作汇报(2)

  29. Reconstruction during 1700--2010 工作汇报(2)

  30. Reconstruction during 1700--2010 工作汇报(2)

  31. Correlation between SN and polar field strength 工作汇报(2)

  32. Relation between SN and total surface flux 工作汇报(2)

  33. Relation between SN and open flux 工作汇报(2)

  34. Comparison of open flux with other reconstructions 工作汇报(2)

  35. Lost cycle? Cy.4: 1784.7 — 1798.3 Usoskin et al. (2009) 工作汇报(2)

  36. Results including the ‘lost cycle’ Against the ‘lost cycle’ 工作汇报(2)

  37. Focus on last 3 cycles (without radial diffusion) 工作汇报(2)

  38. Possible cause of the weak polar field in cycle 23 40% decrease of sunspot number 28% decrease of the sunspot group tilt angle 55% increase of meridional flow 工作汇报(2)

  39. 工作汇报(2)

  40. Jiang et al., 2010, ApJ, 709, 301 Open flux & field strength near Earth Maxima: amplitude; phase difference The disagreement during the minima: strong radial diffusion (100km2s-1)  tilt angle Improved method 工作汇报(2)

  41. Parameter dependence 工作汇报(2)

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