1. The Study of Flows in the Deep Convection Zone (30-200 Mm depth) Tom Duvall Shravan Hanasoge “ASH team”

2. Procedure Three snapshots of ASH simulation flows at r/R=0.72, 0.84, 0.97 Simple interpolation between the depths to create a ‘flow’ model Pass linear waves through the ‘flow’ model Measure travel time shifts at the surface, much as one would with the Sun By doing a similar procedure with the Sun, can see if model is viable.

3. Deep-focusing time-distance helioseismology

6. Azimuthally averaged flows

7. Conclusions Can’t see signals in the Sun at r/R=.95, but can see them from the simulation. Flows in the Sun are not this large?

8. Shortcomings of the present analysis Not a realistic depth variation of the flow. Would need a full 3-d snapshot to have this. Have used ‘noise subtraction’ to measure the simulated flows. This reduces the noise by a factor of ~3. Can’t do this in the Sun, of course.