Deriving the Physical Parameters of a Solar Ejection with an Isotropic Magnetohydrodynamic Evolutionary Model

Details Deriving the Physical Parameters of a Solar Ejection with an Isotropic Magnetohydrodynamic Evolutionary Model Deriving the Physical Parameters of a Solar Ejection with an Isotropic Magnetohydrodynamic Evolutionary Model

Nov 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011apj...741...47b&link_type=abstract

The Astrophysical Journal, Volume 741, Issue 1, article id. 47 (2011).

Astronomy and Astrophysics

Astronomy

Convection, Magnetohydrodynamics: Mhd, Methods: Data Analysis, Plasmas, Sun: Coronal Mass Ejections: Cmes

Scientific paper

The time-space evolution of a ~50° wide coronal mass ejection (CME) on 2007 May 21 is followed remotely with the Solar Terrestrial Relations Observatory heliospheric imager HI-1, and measured in situ near Venus by the MESSENGER and Venus-Express spacecraft. The paper compares the observations of the CME structure with a simple, analytical magnetohydrodynamic force-free solution. It corresponds to a self-similar evolution, which gives a consistent picture of the main spatial-temporal features for both remote and in situ observations. Our main findings are (1) the self-similar evolution allows us to map the CME bright front into about 1/3 of the whole interplanetary counterpart of the coronal mass ejection (ICME, i.e., corresponding to the in situ observed passage of the plasma and magnetic field structure), in good quantitative agreement with the imaging measurements, (2) the cavity following the CME front maps into the rest of the ICME structure, 80% or more of which is consistent with a force free, cylindrically shaped flux rope, and (3) time and space conditions constrain the translational speed of the FR center to 301 km s-1, and the expansion speed of the FR core to 26 km s-1. A careful determination of the ICME cross-section and volume allows us to calculate the mass of the CME bright region (4.3 ± 1.1 1014 g) from the in situ measurements of the proton number density, which we assume to be uniform inside the bright region, of excellent agreement with the value estimated from the SECCHI HI-1 observations for the same structure. We provide model estimates for several global parameters including FR helicity (~2 × 1026 Weber2).

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