A model of a spicule in the solar corona
|1Ladikov-Roev, Yu.P, 1Loginov, AA, 1Maslova, NV, 1Cheremnykh, ОК |
1Space Research Institute of the National Academy of Sciences of Ukraine and the State Space Agency of Ukraine, Kyiv, Ukraine
|Kosm. nauka tehnol. 2004, 10 ;(5-6):128-130|
|Publication Language: Russian|
A stationary model of spicule is considered taking into account the real conditions on the boundaries. We found the relationships between the height of eruption and other main parameters, namely, vertical and azimuthal velocity, value of magnetic field, and density. The existence time of a spicule is estimated.
1. Christopoulou E. B., Georgakilas A. A., Koutchmi S. Fine structure of the magnetic chromosphere: near-limb imaging, data processing and analysis of spicules and mottles. Solar Phys., 199 (1), 61—80 (2001).
2. Sterling A. C. Solar spicules: A review of recent model and targets of future observation. Solar Phys., 196 (1), 79—111 (2000).
3. Whitelam S., Ashbourn J. M. A., Bingham R., et al. Alfven wave heating and acceleration of plasmas in the solar transition region producing jet-like eruptive activity. Solar Phys., 211, 199—219 (2002).