Ubiquitous Solar Eruptions Driven by Magnetized Vortex Tubes

@article{Kitiashvili2012UbiquitousSE,
  title={Ubiquitous Solar Eruptions Driven by Magnetized Vortex Tubes},
  author={Irina N. Kitiashvili and Alexander G. Kosovichev and Sanjiva K. Lele and Nagi N. Mansour and Alan A. Wray},
  journal={arXiv: Solar and Stellar Astrophysics},
  year={2012}
}
The solar surface is covered by high-speed jets transporting mass and energy into the solar corona and feeding the solar wind. The most prominent of these jets have been known as spicules. However, the mechanism initiating these eruptions events is still unknown. Using realistic numerical simulations we find that small-scale eruptions are produced by ubiquitous magnetized vortex tubes generated by the Sun's turbulent convection in subsurface layers. The swirling vortex tubes (resembling… 
Spectro-polarimetric properties of small-scale plasma eruptions driven by magnetic vortex tubes (Special Issue : Recent results from Hinode)
Highly turbulent nature of convection on the Sun causes strong multi-scale interaction of subsurface layers with the photosphere and chromosphere. According to realistic 3D radiative MHD numerical
Solar Vortex Tubes. II. On the Origin of Magnetic Vortices
The solar atmosphere presents a wealth of dynamics due to a constant interplay between the plasma flows and magnetic fields. Twisted flux tubes are an essential magnetic structure, believed to be
Solar Vortex Tubes: Vortex Dynamics in the Solar Atmosphere
In this work, a state-of-the-art vortex detection method, Instantaneous Vorticity Deviation, is applied to locate three-dimensional vortex tube boundaries in numerical simulations of solar
Alfvén Waves in Simulations of Solar Photospheric Vortices
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On the plasma flow inside magnetic tornadoes on the Sun (Special Issue : Recent results from Hinode)
High-resolution observations with the Swedish 1-m Solar Telescope (SST) and the Solar Dynamics Observatory (SDO) reveal rotating magnetic field structures that extend from the solar surface into the
A Three-dimensional Magnetohydrodynamic Simulation of the Formation of Solar Chromospheric Jets with Twisted Magnetic Field Lines
This paper presents a three-dimensional simulation of chromospheric jets with twisted magnetic field lines. Detailed treatments of the photospheric radiative transfer and the equation of states allow
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I. Jet Formation and Evolution due to 3D Magnetic Reconnection
Using simulated data-driven three-dimensional resistive MHD simulations of the solar atmosphere, we show that magnetic reconnection can be responsible of the formation of jets with characteristic of
Dynamic wave-modes in solar chromospheric structures
Sun’s outer atmosphere is a million degree hotter than it’s visible surface, which is not understood with any of the known laws of thermodynamics and remains an intriguing problem for the
Polar Coronal Plumes as Tornado-like Jets
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