Three-dimensional reconstruction of a coronal mass ejection.

Details Three-dimensional reconstruction of a coronal mass ejection. Three-dimensional reconstruction of a coronal mass ejection.

Jul 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995a%26a...299..885j&link_type=abstract

Astronomy and Astrophysics, v.299, p.885

Astronomy and Astrophysics

Astrophysics

16

Sun: Corona, Flares, Solar Wind, Methods: Numerical, Data Analysis

Scientific paper

We reconstruct the three-dimensional density distribution of a coronal mass ejection (CME) in the interplanetary medium from data provided by the Helios spacecraft zodiacal light photometers and by the Solwind coronagraph. Computer assisted tomography (CAT) techniques can be used to reconstruct an image from its projections whenever multiple views of optically thin objects are available. In this case Thomson scattering of sunlight from electrons is the source of variations in observed brightness. Polarization measurements from the Helios spacecraft yield additional information about line of sight electron densities not normally present in usual CAT-scan techniques. The Helios and coronagraph views are not simultaneous; the Helios 16deg photometer observes to within 17Rsun_, whereas the Solwind observations extend outward to only 10Rsun_. However, if we assume radial velocities for ejected material, and that as an approximation the velocity of outward-moving material at a given height is fixed for the ejection, we obtain a solution. This solution is certified by the reconstruction of two test structures - a hollow sphere and two spheres of material analyzed by the same techniques used to deconvolve the CME. The CAT solution shows that the dense structure of the May 7, 1979 CME is distributed in two lobes extending over a quarter of a heliospheric hemisphere. We conclude from the CAT analysis that the CME material must have accelerated from 100km/s in the Solwind field of view to 600km/s in the view from Helios.

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