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Author Feng, Li ♦ Gan, Weiqun ♦ Inhester, Bernd
Source United States Department of Energy Office of Scientific and Technical Information
Content type Text
Language English
Subject Keyword ASTROPHYSICS, COSMOLOGY AND ASTRONOMY ♦ COMPARATIVE EVALUATIONS ♦ GRAVITATIONAL INTERACTIONS ♦ HYDRODYNAMICS ♦ KINETIC ENERGY ♦ LAGRANGIAN FUNCTION ♦ MASS ♦ POTENTIAL ENERGY ♦ SOLAR CORONA ♦ SUN ♦ VELOCITY
Abstract Height–time plots of the leading edge of coronal mass ejections (CMEs) have often been used to study CME kinematics. We propose a new method to analyze the CME kinematics in more detail by determining the radial mass transport process throughout the entire CME. Thus, our method is able to estimate not only the speed of the CME front but also the radial flow speed inside the CME. We have applied this method to a slow CME with an average leading edge speed of about 480 km s{sup −1}. In the Lagrangian frame, the speeds of the individual CME mass elements stay almost constant within 2 and 15 R{sub S}, the range over which we analyzed the CME. Hence, we have no evidence of net radial forces acting on parts of the CME in this range or of a pile up of mass ahead of the CME. We find evidence that the leading edge trajectory obtained by tie-pointing may gradually lag behind the Lagrangian front-side trajectories derived from our analysis. Our results also allow a much more precise estimate of the CME energy. Compared with conventional estimates using the CME total mass and leading edge motion, we find that the latter may overestimate the kinetic energy and the gravitational potential energy.
ISSN 0004637X
Educational Use Research
Learning Resource Type Article
Publisher Date 2015-06-01
Publisher Place United States
Journal Astrophysical Journal
Volume Number 805
Issue Number 2


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