1. GONG 2010 - SoHO 24 A new era of seismology of the Sun and solar-like stars Aix-en-Provence, France Sarbani Basu Yale Unoversity

2. GONG 2004 – SoHO 14 Helio- and Asteroseismology: Towards a Golden Future New Haven, CT, USA

3. The future is here!

4. GONG: Alive and well

6. And after years of waiting in anticipation

7. We can actually do serious asteroseismology now!

8. In fact, we find ourselves drowning in data.

9. Sir Arthur Eddington in “The internal constitution of stars” (1926) “At first sight it would seem that the deep interior of the Sun and stars is less accessible to scientific investigation than any other region of the universe. Our telescopes may probe farther and farther into the depths of space; but how can we ever obtain certain knowledge of that which is being hidden behind substantial barriers? What appliance can pierce through the outer layers of a star and test the conditions within?”

11. The questions have changed. Early concerns for helioseismology were the structure and dynamics of the Sun (the questions that we face in asteroseismology today). Current issues deal with more detailed (and more difficult!) phenomena.

12. Local Helioseismology

13. 6/28/2010 GONG 2010 Aix-en-Provence 3D Inversions Target Depth 1 MmTarget Depth 5 Mm

14. How deep are Sunspots? Acoustic haloes: Surface effect? And what of the discrepancies?

16. Wave-speed below sunspots 1)Results are inconsistent for depths > 2 Mm 2)For all methods and models, except TD: increased wave-speed for depths < 2 Mm.

17. phase-speed filters yield near-surface inflows yield near-surface inflows ridge filters yield near-surface outflows yield near-surface outflows J. Zhao & HMI team A. Birch & D. Braun

18. The question of solar activity and activity related changes Solar oblateness changes, radius does not. Will PICARD confirm this?

19. Is there a 2 nd solar dynamo?

20. Do we really know the microphysics of stars? Could we please, please get our acts together and solve the solar abundance problem? When will the opacity measurement results be available? Please sir, could I have some more (equation of state calculations)?

21. Hey, we can do asteroseismology now!

24. Problems: Mode identification!

25. Stellar activity in mode parameters? The case of HD49933

26. G modes? GOL F Mod el 5.81 σ Adding 5 g modes l=1 (n=-4, -6, -8, -9, -10)

27. Turck-Chièze et al. ApJ 1st June 2010, 715, 1539 On the evolution of the rotation of the young Sun (compared to Bouvier observations) and its present profile obtained for different initial rotation rates A: no braking light blue on left figure, B and C with braking (B: 20km/s on ZAMs navy blue on left figure, C: 50 km/s) and a transport of momentum including diffuive and advective terms, see poster Model-15

28. And what is HMI up to? HMI Optics Package (HOP) OP Structure Telescope Front Window Front Door Vents Support Legs (6) Polarization Selector Focus/Calibration Wheels Active Mirror Limb B/S Alignment Mech Oven Structure Michelson Interf. Lyot Filter Shutters Connector Panel CEBs Detector (Vector) Fold Mirror Focal Plane B/S Mechanical Characteristics: Box: 0.84 x 0.55 x 0.16 m Over All: 1.19 x 0.83 x 0.29 m Mass: 39.25 kg First Mode: 63 Hz Y X Detector (Doppler) Limb Sensor Z

29. HMI Data Products and Objectives Magnetic Shear

30. a) Spectrum of 8 hours of HMI Doppler data near disk center; b) Spectrum of 8 hours of MDI hi-res data (from 1996);

31. Early HMI Magnetic Field Observations Magnetic Field Blos Mean Field HMI – MDI – WSO

32. Early HMI Magnetic Field Observations Frame of Vector Field Movie from Mar 29 Sunspot K. Hayashi, R. Centeno Eliot, et al.

33. Meridional flows from Fourier-Legendre decomposition

34. Spectral Comparison: HMI V vs AIA 1700 (period 2)

35. Dynamos and flows And in the case of massive stars, primordial fields will probably play a large role.

37. Can we detect large scale flows?

39. And what can we look forward to? SONG: Definitely PLATO: We really hope so! Stellar Imager: Solar Orbiter:

40. Issues Theory is lagging behind: how do we deal will waves in a dispersive magnetic medium? Will we be able to detect deeper flows in the Sun? And do the flows look anything like the simulations show? What is the best way to analyze (and model) current data?

41. We shall meet again in Cairns, Australia, Nov 12-16, 2012