http:^^www.cs.wisc.edu^~dailey^abstract.html

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Date: Tue, 05 Nov 1996 00:23:31 GMTServer: NCSA/1.5Content-type: text/htmlLast-modified: Tue, 03 Sep 1996 16:26:39 GMTContent-length: 3034<HTML><HEAD><TITLE>Meridional Motion Abstract</TITLE></HEAD><BODY><H2> Meridional Motions of Magnetic Features in the Solar Photosphere</H2><B> Herschel B. Snodgrass and Sara B. Dailey</B> <BR><BR>Solar Physics <strong>163:</strong> 21-42, 1996<HR><BR><BR><H3> Abstract: </H3>	We cross-correlate pairs of Mt. Wilson magnetograms spaced atintervals of 24-38 days to investigate the meridional motions of smallmagnetic features in the photosphere.  Our study spans the 26-yrperiod July 1967-August 1993, and the correlations determine longitudeaverages of these motions, as functions of latitude and time.  Thetime-average of our results over the entire 26-yr period is, asexpected, antisymmetric about the equator.  It is poleward between ~10degrees and ~60 degrees, with a maximum rate of 13 m/s, but forlatitudes below +/-10 degrees it is markedly equatorward, and it isweakly equatorward for latitudes above 60 degrees.  A running 1-yraverage shows that this complex latitude dependence of the long-termtime average comes from a pattern of motions that changes dramaticallyduring the course of the activity cycle.  At low latitudes the motionis equatorward during the active phase of the cycle.  It tends toincrease as the zones of activity move toward the equator, but itreverses briefly to become poleward at solar minimum.  On the polewardsides of the activity zones the motion is most strongly poleward whenthe activity is greatest.  At high latitudes, where the results aremore uncertain, the motion seems to be equatorward except around thetimes of polar field reversal.  The difference-from-average meridionalmotions pattern is remarkably similar to the pattern of the magneticrotation torsional oscillations.  The correspondence is such that thezones in which the difference-from-average motion is poleward are thezones where the magnetic rotation is slower than average, and thezones in which it is equatorward are the zones where the rotation isfaster.<BR><BR>	Our results suggest the following characterization: there is aconstant and generally prevailing motion which is perhaps everywherepoleward and varies smoothly with latitude.  On this is superimposed acycle-dependent pattern of similar amplitude in which the meridionalmotions of the small magnetic features are directed away from regionsof magnetic flux concentration.  This is suggestive of simplediffusion, and of the models of Leighton(1964) and Sheeley, Nash, andWang(1987).  The correspondence between the meridional motions patternand the torsional oscillations pattern in the magnetic rotationsuggests that the latter may be an artifact of the combination ofmeridional motion and differential rotation.<BR><BR><BR><LI> <I>Herchel Snodgrass is a professor at Lewis and Clark College.</I><BR><LI> <I>Sara (Dailey) Bauman is a graduate student at the Univ. of Wisconsin - Madison</I><BR><BR><HR><BR><address><!WA0><!WA0><!WA0><!WA0><a HREF="http://www.cs.wisc.edu/~dailey/dailey.html"> dailey@cs.wisc.edu </a> <BR>Tues Sept 3 1996 </BODY></HTML>

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