Speaker
Haruhisa Iijima
(Institute for Space-Earth Environmental Research (ISEE), Nagoya University)
Description
A three-dimensional simulation by the Tokyo code (tentative name) is presented to
investigate the effect of three-dimensionality on the scale of chromospheric jets and
the dependence on the photospheric magnetic field structure. We newly develop a
numerical code for the radiation magnetohydrodynamic modeling of solar atmosphere.
The code includes the effect of non-local radiative transfer in the photosphere and
optically thin radiative cooling in the upper layer. The Spitzer-type thermal
conduction and latent heat of partial ionization is also taken into account. The tall
chromospheric jets with the maximum height of 10–11 Mm and lifetime of 8—10 min are
formed above the strong magnetic field concentration. The strongly entangled magnetic
field lines are formed in the chromosphere, which helps to drive these tall
chromospheric jets through the Lorentz force. We also find that the produced
chromospheric jets form a cluster with the diameter of several Mm with finer strands.
Primary author
Haruhisa Iijima
(Institute for Space-Earth Environmental Research (ISEE), Nagoya University)
