High
spatial and temporal resolutions of the Solar Optical Telescope (SOT) on board Hinode enabled us to capture fast dynamic phenomena
caused by flux emergence. One such phenomenon may be a chromospheric running wave from a
rotating magnetic polarity region with a size of > 5,000 km (hereafter, solar cyclone compared to a cyclone on the Earth). A possible mechanism for
producing the running wave was investigated with a three-dimensional
MHD simulation of an emerging twisted flux tube. The simulation showed that the solar cyclone formed an arc-shaped chromospheric region with enhanced plasma density in front of it, which propagated outward from the core of the cyclone where a strong downdraft was generated along magnetic field lines locally standing vertical.
Reference
Magara, T. et al. 2012 PASJ, 64, L4
Wedemeyer-Bohm, S., & Rouppe van der Voort, L. 2009, A&A, 507, L9
Kitiashvili, I. N., et al. 2012, ApJ, 751, L21
movie version
(gold thick line... magnetic field line, thin arrowed green line... flow vector)
movie version
