Large-scale velocity fields and small-scale magnetic fields during the maximum of solar cycle 22

Details Large-scale velocity fields and small-scale magnetic fields during the maximum of solar cycle 22 Large-scale velocity fields and small-scale magnetic fields during the maximum of solar cycle 22

Feb 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994cait.reptq....m&link_type=abstract

Final Report, 1 Oct. 1989 - 30 Sep. 1993 California Inst. of Tech., Pasadena. Solar Astronomy Group.

Physics

Magnetic Field Inversions, Size Distribution, Solar Activity, Solar Cycles, Solar Magnetic Field, Solar Physics, Velocity Distribution, Dynamo Theory, Magnetic Poles, Solar Activity Effects, Solar Flares, Solar Prominences

Scientific paper

Studies of the solar cycle have revealed that the size distribution of active regions does not vary with the solar cycle. Size, rate of rise, and lifetime of active regions are roughly proportional although a wide range of variation exists among these parameters. The polar field typically reverses about 2 years after solar maximum. The new solar cycle does not seem to start until after the reversal of the sign of the magnetic poles. However, the new solar cycle does overlap appreciably with the previous cycle and begins 3 or more years prior to the minimum in sunspot producing active regions. The solar cycle begins with ephemeral regions at high latitudes. From the analysis of active region and ephemeral region data over more than a whole solar cycle it is concluded that ephemeral regions are in all respects the small-scale end of the distribution of active regions. No rationale was found for excluding ephemeral regions as one of the effects of the solar dynamo. The search for the early ephemeral regions associated with solar cycle 23 at high latitudes yielded the tentative conclusion that it was detected during our observing runs during the spring of 1993 although confirming data is needed.

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