http://arxiv.org/abs/1412.2964
As the most energetic eruptions in the solar system, coronal mass ejections (CMEs) can produce shock waves at both their front and flanks as they erupt from the Sun into the heliosphere. However, the amount of energy produced in these eruptions, and the proportion of their energy required to produce the waves, is not well characterised. Here we use observations of a solar eruption from 2014 February 25 to estimate the energy budget of an erupting CME and the globally-propagating “EIT wave” produced by the rapid expansion of the CME flanks in the low solar corona. The “EIT wave” is shown using a combination of radio spectra and extreme ultraviolet images to be a shock front with a Mach number greater than one. Its initial energy is then calculated using the Sedov-Taylor blast-wave approximation, which provides an approximation for a shock front propagating through a region of variable density. This approach provides an initial energy estimate of $\approx$2.8$\times$10$^{31}$ ergs to produce the “EIT wave”, which is approximately 10% the kinetic energy of the associated CME (shown to be $\approx$2.5$\times$10$^{32}$ ergs). These results indicate that the energy of the “EIT wave” may be significant and must be considered when estimating the total energy budget of solar eruptions.
D. Long, D. Baker, D. Williams, et. al.
Wed, 10 Dec 14
9/61
Comments: 12 pages, 6 figures. Accepted for publication in The Astrophysical Journal