and SOT Magnetogram Analysis
of the Small-scale Magnetic Elements
in a Solar Emerging Flux Region
||456, The Fifth Hinode Science Meeting
||Toriumi, S.; Yokoyama, T.
||In this study,
we aim to figure out the flux emergence
from the interior to the atmosphere
through the surface,
by conducting a numerical simulation
and a Hinode/SOT observation.
First, we performed a three-dimensional
magnetohydrodynamic (MHD) simulation
on the flux tube emergence
from –20,000 km
of the convective layer.
As a result, the rising tube expands
sideways beneath the surface
to create a flat structure.
As time goes on,
the subphotospheric field rises again into the corona
the magnetic buoyancy instability.
We newly found that the photospheric magnetogram
shows multiple separation events
as well as shearing motions,
which reflects the Parker instability
of the subphotospheric field.
This situation agrees well with
Strous & Zwaan (1990)'s model
based on their observation.
We also confirmed that the wavelength
perpendicular to the separations
is approximately a few times
the tube's initial radius.
Secondly, we analyzed SOT/FG magnetogram
of AR 10926,
and observed that the small-scale magnetic elements
among the major sunspots
make alignments with a certain orientation.
The wavelength perpendicular to the alignments
was found to be ∼3,000km.
Comparing with the numerical results,
we speculate that this active region
observed by the SOT is created
by the rising flux tube
with a radius of the order
of 1,000 km
in the deeper convection zone.