Reconstruction of CME-Driven Shocks Using STEREO Observations

Details Reconstruction of CME-Driven Shocks Using STEREO Observations Reconstruction of CME-Driven Shocks Using STEREO Observations

May 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009spd....40.2212v&link_type=abstract

American Astronomical Society, SPD meeting #40, #22.12; Bulletin of the American Astronomical Society, Vol. 41, p.860

Astronomy and Astrophysics

Astronomy

Scientific paper

Recent work has shown that CME-driven shocks can easily be detected by white light coronagraph observations from a few solar radii above the surface to at least 20 Rs. However, the shock emission suffers from the same projection effects at the CME emission making precise measurements of the shock properties difficult and prone to assumptions. The two viewpoint observations from the SECCHI/COR2 coronagraphs aboard the STEREO mission offer an unprecedented opportunity to reconstruct the 3D envelope of the shock using the same procedures applied to the successful reconstruction of the CME itself. Due to the low solar activity over the last years, there have been only a handful of white lght shock candidates observed with SECCHI. We examine the most prominent one, associated with the eruption on December 31, 2007. We find that the shock does not evolve isotropically but it is influenced by the large scale coronal magnetic field configuration. To study this interaction in more detail, we employ a sophisticated thermodynamic model of the corona to derive a 3d distribution of the Alfvén speed around the eruption site. We find that we can account for the coronagraph observations only if the shape of the shock closely matches that of the surrounding magnetic field.

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