1. Rachel Howe

2.  Why do we need to continue observing?  Why ground-based?  Requirements for a new network

4. Dynamics changes – rotation-rate variations Part of the puzzle for the dynamo Useful for “preview” of activity cycle timing

5.  Or so we thought …

6. Rotation-rate variations near the tachocline

7. Torsional oscillation from ring-diagram analysis: MDI-GONG combo that I showed at the AGU meeting. MDI before mid-2001, GONG after. The flows are averaged in depth over 4-10 Mm. Bands of faster (or slower) rotation move toward the equator. The fast band of cycle 24 appears before there is any surface activity present. The new fast band is stronger in the northern hemisphere indicating that the activity will be stronger in this hemisphere. Courtesy of R. Komm

8. Figure 2 from Meridional Circulation During the Extended Solar Minimum: Another Component of the Torsional Oscillation? I. González Hernández et al. 2010 ApJ 713 L16 doi:10.1088/2041- 8205/713/1/L16 Temporal variation of the fitted polynomial to the meridional circulation observations at a depth of 5.8 Mm. (Bottom panel symmetrized; poleward velocities positive.)

9.  ACRIM (Woodard & Noyes 1985, 1988, Gelly, Fossat & Grec 1988)  BiSON, Mark I (Palle et al. 1989, Elsworth et al. 1990) Chaplin et al. 2007

10. Normalized even-a coefficients vary as Legendre decomposition of magnetic field distribution

11. Normalized even-a coefficients vary as Legendre decomposition of magnetic field distribution – but fit isn’t perfect; residuals correlated between GONG, MDI

12. Localized GONG frequency shifts

14. Redundancy/ease of repair -- lose one site for a few months, still get usable data

15.  Longevity BiSON – courtesy W. Chaplin

16.  Redundancy

18.  Minimum for global: continuation of GONG classic cadence/resolution/duty cycle  For local:  > 75% duty cycle,  <0.1 deg angular drift  Overlap between sites for cross-calibration  Minimum 1-year overlap with predecessor  Improved peak fitting

19.  Work for example with AIA UV intensity has shown how mode behavior varies through the atmosphere

22. HMI V HMI Ic HMI Lc AIA 1700 3mHz 5mHz 7mHz