||Is There Observational Evidence Indicating a Small-Scale Solar Dynamo?
||455, 4th Hinode Science Meeting: Unsolved Problems and Recent Insights
||Lites, B. W.
||Observations from the Hinode/SOT
spectro-polarimeter are examined with the aim of identifying
diagnostics for the presence (or absence) of a self-sustained
small-scale turbulent dynamo in the upper solar convection zone. We
examine 45 Hinode data sets obtained during 2007. We find
much smaller net flux imbalance within regions of the quiet Sun having
very weak flux compared to the imbalance averaged over each data set.
Further, there is no correlation of the average net unsigned flux of
regions having very weak flux relative to the average unsigned flux of
the entire region. If internetwork fields were to arise from
dispersal of flux from active regions, one would expect both measures
to show significant correlation, so this analysis strongly supports
the small-scale dynamo scenario. We also find that the average of the
longitudinal apparent flux density increases slightly toward the limb
for the very weakest observed flux elements. This behavior is likely
the result of the dominance of horizontal fields higher in the
photosphere. From data with very high signal-to-noise ratio, the
distribution of magnetic field strength indicates that the magnetic
energy of the quiet Sun is dominated by the small fraction of field
elements having kG strengths. These strong-field elements are
responsible for most of the imbalance of magnetic flux measured in
each region, so it is suggested that they arise primarily from
dispersal of flux from active regions, not from a small-scale dynamo.