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Journal of Physical Studies 16(1/2), Article 1901 [8 pages] (2012)
DOI: https://doi.org/10.30970/jps.16.1901 PROPERTIES OF CORONAL MASS EJECTIONS PROPAGATING IN THE HELIOSPHEREG. A. Porfir'eva, G. V. Yakunina
State Sternberg Astronomical Institute, |
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Propagating through the heliosphere coronal mass ejection (CME) could change its direction and velocity. The direction of propagation of a CME defines if the CME would arrive in the Earth or not. The data on the propagation of coronal mass ejections (CMEs) registered in recent decades have been collected. The results of white-light observations with the LASCO SOHO and instruments onboard STEREO A and B spacecrafts are used. In the nearest corona velocities of different CMEs may range from $(2-3)\times 10^2$ km s$^{-1}$ to $(4-5)\times 10^2$ km s$^{-1}$ up to $(1-3)\times 10^3$ km s$^{-1}$ for the fastest ones. Propagating through the solar corona CMEs change their shapes demonstrating self-similar expansion, flattening or no expansion. At an early stage CMEs might deflect in the meridional direction for $\sim(2^{\circ}-30^{\circ})$ from high latitudes to the heliospheric current sheet (HCS). Simultaneous observations from STEREO A and B have shown the azimuthal deflection for $5^{\circ}-30^{\circ}$ up to the distances of 40-70 $R_{☉}$. The models explaining the observed phenomena of CMEs deflections are briefly discussed.
PACS number(s): 96.60.ph