Subsurface Convective Flows within Active Regions
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Subsurface Convective Flows within Active Regions
Bradley W. HindmanDeborah A. Haber
Juri Toomre
JILA/University of Colorado
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Ring Power Spectra
The modes appear as nested trumpets aligned with the frequency axis.
Cuts at constant frequency produce nested rings that have larger radii for larger frequencies.
Changes in the mode frequencies manifest as changes to the radii of the rings. Therefore, careful measurement of the radii can be used to determine subsurface structure (sound speed, gas pressure, etc.).
f mode
p1 mode
p2 mode
p3 mode
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The Effects on p-mode Spectra
TrackedTracked Not TrackedNot Tracked
The above spectra was obtained bystudying the same area on the solardisk. Equatorial rotation results in a speed of ~ 2000 m/s.
This above spectra was obtained by following the same patch of fluid as it rotates across the solar disk. This removes the large rotational velocity.
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High-Resolution Ring Analysis (HRRA)
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Low-Resolution MappingInflow nearthe surface
Outflow atdepth
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High-Resolution Mapping
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Flows Around an Active Region
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Newly Emerged Region
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Smoothed Magnetogram
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Contours of the Smoothed Magnetogram
50 G
100 G
150 G
200 G
250 G
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InflowsInflow
Outflow
Outflow
Inflow
NOAO 9433
Average of all active regions March 29 – April 24, 2002 [03/29 – 05/21]
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Divergence and Curl
Average of all active regions March 29 – April 24, 2002 [ 03/29 – 05/21].◊ 50 G contour◊ 100 G contour◊ 150 G contour◊ 200 G contour
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Conclusions
• The boundaries of active regions are zones of inflow, with typical inflow speeds of 20 m/s.
• The cores of active regions generally possess strong outflows (50 m/s), probably the result of outflows from sunspots.
• We see no evidence for systematic vertical vorticity within active regions. (At least at the spatial scale sampled by out HRRA technique.)