1. Magnetic fields in the photosphere and heliosphere: structure, statistical parameters, turbulent state Valentyna I. Abramenko Big Bear Solar Observatory of NJIT Email: avi@bbso.njit.eduavi@bbso.njit.edu http://www.bbso.njit.edu/~avi/

2. Outlook Analysis of line-of-sight magnetograms: - Magnetic energy dissipation structures - Magnetic power spectrum: flare productivity forecast Analysis of the parameters of coronal holes: - Dipole emergence rate in coronal holes - Magnetic Power Spectrum: expansion into the heliosphere Distributions of the magnetic field discontinuities in the solar wind ACE data

3. Magnetic energy dissipation structures  Abramenko, Yurchyshyn, Wang H., Spirock, Goode 2003, ApJ 597

4. Coronal Heating High magnetic energy dissipation rate in the photosphere is associated with high temperature and emission measure in the corona. Abramenko, Pevtsov, Romano 2006 ApJ 646

5. Magnetic Power Spectrum: Flare-quiet active region 0061Flaring active region 9077

6. PS(corrected) = PS(Full Disk) / Correction Function Correction Function = PS (Full Disk) / PS (High Res)

7. Emerging Active Region 0488 The power index peaked by the end of the first day of AR’s life, while the magnetic flux has saturated by the end of the 3 rd day flarecontaminatedmeasurements 15h

8. Soft X-ray Flare Index versus Magnetic power index Abramenko 2005, ApJ, 629

9. Further study of photospheric magnetograms Separate study of emerging ARs Power spectrum from magnetograms obtained with SDO and Solar B ( possibility for extension of the inertial range, for study of the dissipation range?) Power spectra from different areas on the Sun (ARs, plage areas, Quiet Sun areas, CHs) Structure Functions and Filling Factor in different areas on the Sun

10. Collaborations in frameworks of the Heliospheric Focus Team Study of the magnetic field parameters inside coronal holes (collaboration with L.A.Fisk and T. Zurbuchen) Analysis of the statistical parameters of the solar wind data (collaboration with B.Vasquez and D.Haggerty)

11. The Rate of Emergence of Magnetic Dipoles in Coronal Holes and Outside

12. In all cases, the dipole emerging rate for CHs is lower than that for adjacent QS areas (all data points are above the bisector). This implies that a coronal hole is a region with a local minimum in the rate of emerging dipoles

13. This result supports the concept that reconnection of open field lines with coronal loops is an important transport mechanism on the Sun (Fisk 2005), and needs to be included in models for the evolution of the solar magnetic field. The dipole emergence rate in Quiet-Sun areas exceeds approximately twice that in Coronal Holes. This implies that a coronal hole is a region with a local minimum in the rate of emerging dipoles.