2 research outputs found
The Interaction of New and Old Magnetic Fluxes at the Beginning of Solar Cycle 23
The 11-year cycle of solar activity follows Hale's law by reversing the
magnetic polarity of leading and following sunspots in bipolar regions during
the minima of activity. In the 1996-97 solar minimum, most solar activity
emerged in narrow longitudinal zones - `active longitudes' but over a range in
latitude. Investigating the distribution of solar magnetic flux, we have found
that the Hale sunspot polarity reversal first occurred in these active zones.
We have estimated the rotation rates of the magnetic flux in the active zones
before and after the polarity reversal. Comparing these rotation rates with the
internal rotation inferred by helioseismology, we suggest that both `old' and
`new' magnetic fluxes were probably generated in a low-latitude zone near the
base of the solar convection zone. The reversal of active region polarity
observed in certain longitudes at the beginning of a new solar cycle suggests
that the phenomenon of active longitudes may give fundamental information about
the mechanism of the solar cycle. The non-random distribution of old-cycle and
new-cycle fluxes presents a challenge for dynamo theories, most of which assume
a uniform longitudinal distribution of solar magnetic fields.Comment: 4 pages, 5 figures; accepted for publication in ApJ Letter
Active region formation through the negative effective magnetic pressure instability
The negative effective magnetic pressure instability operates on scales
encompassing many turbulent eddies and is here discussed in connection with the
formation of active regions near the surface layers of the Sun. This
instability is related to the negative contribution of turbulence to the mean
magnetic pressure that causes the formation of large-scale magnetic structures.
For an isothermal layer, direct numerical simulations and mean-field
simulations of this phenomenon are shown to agree in many details in that their
onset occurs at the same depth. This depth increases with increasing field
strength, such that the maximum growth rate of this instability is independent
of the field strength, provided the magnetic structures are fully contained
within the domain. A linear stability analysis is shown to support this
finding. The instability also leads to a redistribution of turbulent intensity
and gas pressure that could provide direct observational signatures.Comment: 19 pages, 10 figures, submitted to Solar Physic