|Author||Iijima, H. ♦ Yokoyama, T.|
|Source||United States Department of Energy Office of Scientific and Technical Information|
|Subject Keyword||ASTROPHYSICS, COSMOLOGY AND ASTRONOMY ♦ CHROMOSPHERE ♦ CONVECTION ♦ ELEMENT ABUNDANCE ♦ EQUATIONS OF STATE ♦ LIFETIME ♦ LORENTZ FORCE ♦ MAGNETIC FIELDS ♦ MAGNETOHYDRODYNAMICS ♦ QUANTUM ENTANGLEMENT ♦ RADIANT HEAT TRANSFER ♦ SIMULATION ♦ SOLAR PROMINENCES ♦ SUN ♦ SURFACES ♦ THREE-DIMENSIONAL CALCULATIONS|
|Abstract||This paper presents a three-dimensional simulation of chromospheric jets with twisted magnetic field lines. Detailed treatments of the photospheric radiative transfer and the equations of state allow us to model realistic thermal convection near the solar surface, which excites various MHD waves and produces chromospheric jets in the simulation. A tall chromospheric jet with a maximum height of 10–11 Mm and lifetime of 8–10 minutes is formed above a strong magnetic field concentration. The magnetic field lines are strongly entangled in the chromosphere, which helps the chromospheric jet to be driven by the Lorentz force. The jet exhibits oscillatory motion as a natural consequence of its generation mechanism. We also find that the produced chromospheric jet forms a cluster with a diameter of several Mm with finer strands. These results imply a close relationship between the simulated jet and solar spicules.|
|Learning Resource Type||Article|
|Publisher Place||United States|
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