Parker Instability(Winter School 2006)
Emerging Flux in Solar Atmosphere
How to use computers in Winter School 2006 #3
initial condition setting program(model.f) within comment
simulation files (packed tar and gzip)
file of presentation(for OpenOffice)
file of presentation(for PowerPoint)
PDF file of presentation
Shibata's Emerging Model

Shibata et al.(1989)
Shibata et al.(1989)[PDF file]
3D results

Nozawa(2005)
Nozawa(2005)[PDF file]
The magnetic flux expands horizontally when the magnetic field
emerges into the photosphere, because the velocity is estimated
by assuming that the kinetic energy is equal to the magnetic energy.
Lifetime ~ 10-30min, Velocity ~ 10km/s(sound velocity)
The velocity was estimed:
rho v^2 ~ B^2/(8pi) ... kinetic energy is balanced to magnetic energy
:
Pv^2/Cs^2 ~ B^2/(8pi) (rho=P/Cs^2)
v^2 ~ B^2/(8pi P) Cs^2 ~ 1/beta Cs^2
---> mistake ?
Now let's think what has determined the expand velocity ?
Next figure is hint ???
grad B^2/(8pi) + grad rho v^2 + grad P + rho g + B^2/(4pi R) = constant

SMART(Solar Magnetic Activity Research Telescope) in Hida Observatory of Kyoto Univ.

19-Aug-2005 2:50-6:30 UT(5,10,20km/s)
movie
Ha Observation(0.2-1km/s(sometimes 5km/s)

Georgakilas et al.(1993)
Georgakilas et al.(1993)[PDF file]
Parker Instability 3D Simulation

Matsumoto et al.(1993)
Matsumoto et al.(1993)[PDF file]
Parker Instability 2D Simulation

Magara(2001)
Magara(2001)[PFD file]
example result in this project

parameter(Magnetic Strength, Coronal height, etc)
By means of magnetohydrodynamic simulations, we study nonlinear
evolutions of the magnetic buoyancy instability such as the Parker
instability in a gravitationally stratified magnetized gas layer.
You will set up initial conditions for the Galaxy or for the Sun,
and simulate the growth of the instability. We discuss how the
magnetic loops created by the instability will actually be observed.