Abstract
A brief review of results of observations of coronal mass ejections (CMEs), obtained aboard SOHO and STEREO during last decades, is presented. CMEs velocity, acceleration, mass and angular width are considered in connection with the flares arising simultaneously with the CMEs from common solar regions. Statistically properties of associated CMEs-flares are related. So, higher the flux of the associated flare is, higher the CME mass, angular width and velocity are. The magnetic helicity of an active region (AR) seems to play an important role whether a confined or a CME-associated flare will be produced. The dynamical evolution of CMEs shows that the total energy is kept relatively constant and the energy released in radio and other forms of radiations is not significant. Slow CMEs could propagate through heliosphere with a deflection of \(2 - 3{0}^{\circ }\) both in latitudinal and azimuthal direction obeying an interaction with the surrounding magnetic field. Faster CMEs tend to propagate radially. Data from published scientific papers and Internet have been used.
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The work was supported by the Russian Foundation for Basic Research grant No 11–02–00843 and by grants OFN-15 and NSH-3645.2010.2.
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Porfir’eva, G.A., Yakunina, G.V., Borovik, V.N., Grigoryeva, I.Y. (2012). Coronal Mass Ejections on the Sun and Their Relationship with Flares and Magnetic Helicity. In: Obridko, V., Georgieva, K., Nagovitsyn, Y. (eds) The Sun: New Challenges. Astrophysics and Space Science Proceedings, vol 30. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-642-29417-4_21
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