Can we use nonlinear and selfconsistent models for data analysis?

1. Can we use nonlinear and selfconsistent models for data analysis? Thomas Wiegelmann • We learned from Prof. Schindler about the importanceof nonlinear and selfconsistent models. • Karl Schindler also introduced me to observational data(Helmetstreamer and coronal mass ejections observedwith SOHO/LASCO) and encouraged me to develop a corresponding 2D MHD model under his supervision. • New aspects: - Feed models directly with measured data. - Computations in 3D.

2. Example: Coronal magnetic fields • We cannot measure coronal magnetic fields directly. • Extrapolate the coronal magnetic fields from photospheric (vector) magnetograms. • Needed: Model assumptions regarding the coronal plasma. • Use the reconstructed magnetic field model to supportdata analysis, e.g., - Coronal images (SOHO, Solar-B) - Doppler maps (SOHO/Sumer) - Stereoscopy (STEREO-mission) - Tomography (STEREO-mission)

3. Coronal magnetic field models

4. Active regions contain mainly closed magnetic loops. Coronal plasma is trapped in closed loops and causes bright emission. The large scale magnetic field structure in coronal holes is open. The coronal plasma escapes along open field lines (solar wind). and the emissivity in coronal lines is strongly reduced here.

5. Coronal Holes (Wiegelmann & Solanki, Sol. Phys. 2004) EIT 195 Fe XIIFormation temperature 1.5 million K EIT 304 He IIFormation temperature 60,000-80,000 K

7. Use RTV scaling laws to approximate temperatures T ~ (pL)1/3 The emitting volume filled by gas at that temperature corresponds to the emitted radiation. In CH ~70% at low and ~10% at high temperatures compared with the quiet Sun.

8. Active Regions (Marsch, Wiegelmann & Xia, A&A 2004) EIT-image and projections of magnetic field lines for a potential field (α=0). (bad agreement) Linear force-free field with α=+0.01 [Mm-1] (bad agreement) We use a linear force-free model with MDI-data and have the freedom to choose an appropriate value for the force-free parameter α.

9. Linear force-free field with α=-0.01 [Mm-1] (better agreement) 3D-magnetic field lines, linear force-free α=-0.01 [Mm-1]

10. down up Mass flux density inferred from Doppler- shift and intensity from SUMER observations. SUMER Dopplergram in NeVIII ( 77 nm) and a 2-D-projection of some field lines.

11. Nonlinear force-free fields • Why do we need nonlinear force-free fields?- Non magnetic forces are small in the corona. - Potential and linear force-free fields are to simple to estimate free energy and magnetic topology. • The computation is much more difficult:- Mathematical difficulties due to non-linearity.- Vector magnetograms are not force-free.- Transversal B-field is very noisy.- Limited field of view for current instruments (SFT/Tokyo, VTT/Tenerife, IVM/Hawaii)

13. Preprocessing of non-force-free and noisy magnetograms. (Wiegelmann, Inhester, Sakurai 2006, using force-free consistency criteria developed by Aly 1989)

15. Test the nonlinear force-free extrapolations with Low&Lou 1990 equilibrium. a: Reference, b: Potential field, c: Reconstruction from noisy data. d: Reconstruction from preprocessed noisy data

16. Preprocessing of vector magnetograms helps to diminish inconsistencies and noise. (Wiegelmann, Inhester, Sakurai, Sol. Phys. 2006)

17. Comparison of observed magnetic loops and extrapolations from the photosphere with different models. Potential field reconstruction Linear force-free reconstruction Non-linear force-free reconstruction Measured loops in a newly developed AR (Solanki, Lagg, Woch, Krupp, Collados, Nature 2003)

18. We compared measurements of magnetic loops in a newly developed active region with extrapolations from the photosphere. We got the best agreement of measured and extrapolated loops for a non-linear force-free magnetic field model. (Wiegelmann, Lagg, Solanki, Inhester, Woch, A&A 2005)

20. Magnetic fields and coronal tomography • Use only line of sight density integrals. b) Use only magneticfield data. c) Use both line of sightdensity integrals andmagnetic field as regularization operator. (Wiegelmann and Inhester, Sol. Phys., 2003)

21. Near Future: STEREO-mission Two almost identical spacecrafts will observe the Sun and solar wind Markus Aschwanden: Since the STEREO mission is our first extensive multi-spacecraft 3D exploration of our heliosphere, its importance might be compared with the first determination of the true 3D geometry of our Earth globe, thaught by Thales of Milet and Pythagoras around 600 BC. • Launched 25.October 2006. • Spacecrafts have different orbits due to Swing-by at moon. • The two STEREO spacecrafts separate about 44o every year. • More than 2GB data every day. PhD students at the MPS in Lindau: - Li Feng: Stereoscopy of Active Regions. - Peng Ruan: Global model of the corona.

22. Li Feng: Stereoscopy of Active Regions Optimal linear force-free model (black) and coronal loops (red) from two viewpoints. 2000-3-1 14:22 3-2 17:44 TRACE EUV images Classical Stereoscopy Magnetic Stereoscopy

23. Peng Ruan: Global coronal modeling • Compute global magnetic • field with different models: • Potential and LFF fields • MHS (Neukirch 95 model) • Compute the coronal plasma • with the help of Scaling Laws (Schrijver et al 2004) • or selfconsistently from • MHS model. • Compare artificial coronal images with real images • from 2 Stereo viewpoints. • Aim: Find optimal model parameter set. Temperature distribution in the solar corona cut through longitude Ø=40o and 220o

24. Conclusions • Potential magnetic fields and linear force-free fields are popular due to their mathematic simplicity and available data. (e.g. from MDI on SOHO, Kitt Peak) • Non-linear force-free fields are necessary todescribe active regions exactly. More challenging both observational (vector magnetographs) and mathematical. • Vector magnetograms with high spatial and temporal resolution become available soon (SOLIS, Solar-B, SDO, Solar Orbiter).

25. Thank you very much to Prof. Karl Schindler