Radial Flows in Supergranules

Details Radial Flows in Supergranules Radial Flows in Supergranules

Jan 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002soph..205...25h&link_type=abstract

Solar Physics, v. 205, Issue 1, p. 25-38 (2002).

Physics

25

Scientific paper

We determine the radial component of the supergranular flow velocity by examining the center-to-limb variation of the Doppler velocity signal. We acquire individual Doppler images obtained with the MDI instrument on the SOHO spacecraft and process them to remove the p-mode oscillation signal, the axisymmetric flows, the convective blueshift signal, and instrumental artifacts. The remaining Doppler signal contains only non-axisymmetric flow structures. The Doppler signal from the horizontal flows in these structures varies like sinρ, where ρ is the heliocentric angle from disk center. The Doppler signal from radial flows varies like cosρ. We fit the center-to-limb variation of the mean squared velocity signal to a straight line in sin^2ρ over the central portion of the disk. The intercept of this line at disk center gives the amplitude of the radial component of the flow. The slope of the line gives the amplitude of the horizontal component. We find that the radial flows for typical supergranules have speeds about 10% that of their associated horizontal flows or about 30 m s^-1. The ratio of the radial to horizontal flow speed increases from 9% to about 18% as the size of the structure decreases from >60 Mm to ~5 Mm. We use data simulations to check these results and find a ratio that increases from 5% to only about 12% over the same range of sizes. These smaller ratios are attributed to an underestimation of the horizontal flow speeds due to the fact that the transverse component of the horizontal flow is not detected by Doppler measurements.

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