Kinematics of coronal mass ejections between 2 and 30 solar radii. What can be learned about forces governing the eruption?

Details Kinematics of coronal mass ejections between 2 and 30 solar radii. What can be learned about forces governing the eruption? Kinematics of coronal mass ejections between 2 and 30 solar radii. What can be learned about forces governing the eruption?

Aug 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004a%26a...423..717v&link_type=abstract

Astronomy and Astrophysics, v.423, p.717-728 (2004)

Astronomy and Astrophysics

Astrophysics

42

Magnetohydrodynamics (Mhd), Sun: Corona, Sun: Coronal Mass Ejections (Cmes), Sun: Solar-Terrestrial Relations, Sun: Solar Wind, Interplanetary Medium

Scientific paper

Kinematics of more than 5000 coronal mass ejections (CMEs) measured in the distance range 2-30 solar radii is investigated. A distinct anticorrelation between the acceleration, a, and the velocity, v, is found. In the linear form, it can be represented as a=-k1(v-v0), where v0=400 km s-1, i.e., most of CMEs faster than 400 km s-1 decelerate, whereas slower ones generally accelerate. After grouping CMEs into the width and mean-distance bins, it was found that the slope k1 depends on these two parameters: k1 is smaller for CMEs of larger width and mean-distance. Furthermore, the obtained CME subsets show distinct quadratic-form correlations, of the form a= -k2 (v-v0)| v-v0|. The value of k2 decreases with increasing distance and width, whereas v0 increases with the distance and is systematically larger than the slow solar wind speed by 100-200 km s-1. The acceleration-velocity relationship is interpreted as a consequence of the aerodynamic drag. The excess of v0 over the solar wind speed is explained assuming that in a certain fraction of events the propelling force is still acting in the considered distance range. In most events the inferred propelling force acceleration at 10 solar radii ranges between aL=0 and 10 m s-2, being on average smaller at larger distances. However, there are also events that show aL>50 m s-2, as well as events indicating aL<0. Implications for the interplanetary motion of CMEs are discussed, emphasizing the prediction of the 1 a.u. arrival time.
Appendices A and B are only available in electronic form at http://www.edpsciences.org

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