The Sun rings like a bell. By looking at the frequencies of this
ringing we can tell what the bell is made of. In the case of the
Sun we can tell the sound speed (temperature) of the gas, rotational
velocities, plus other properties, all as a function of depth. In
essence we can look inside the Sun by studying its vibrations. What
is it that rings the bell by exciting the oscillations? Probably
convective motions. Supersonic downdrafts may also play a role.
Researchers in NCAR’s High Altitude Observatory division are attempting
to better understand the processes that may influence the acoustical
properties of the Sun. Using complex numerical models, the effects
of ionization on the dynamics and transport properties of a compressible,
convective fluid are being studied.
The fluid in these experiments is pure hydrogen. Experiment conditions
are intended to be similar to those of the solar convection zone.
Unlike conditions in the Sun, however, only a fraction of the hydrogen
is permitted to ionize. The model becomes numerically unstable when
100% ionization occurs. As the fraction of fluid permitted to ionize
increases, convective down flows become more vigorous, reaching
supersonic velocities. For an ionization fraction of .25, average
peak velocities reach Mach 1.2. For an ionization fraction of zero
(an ideal gas), peak vertical velocities only average around 0.5.
For f>0.5, the down flows become so vigorous that they become
unresolvable using present 256^3 numerical simulations. The existence
of these supersonic down flows may have implications for heat transport
and solar acoustic oscillations
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The animation depicts two views of an H2 ionization
field, one from below and one from above. Red (near the top) indicates
areas of low ionization. Yellow, near the bottom, shows areas of
high ionization. As bouncy drives the cool, dense H2 downward, heat
causes the gas to ionize. Periodically a downward plume will reach
supersonic velocities. These supersonic plumes are shown in green. |