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The most intense solar energetic particle events are produced by coronal massejections (CMEs) accompanied by intense type II radio bursts below 15 MHz.Understanding where these type II bursts are generated relative to an eruptingCME would reveal important details of particle acceleration near the Sun, butthe emission cannot be imaged on Earth due to distortion from its ionosphere.Here, a technique is introduced to identify the likely source location of theemission by comparing the observed dynamic spectrum observed from a singlespacecraft against synthetic spectra made from hypothesized emitting regionswithin a magnetohydrodynamic (MHD) numerical simulation of the recreated CME.The radio-loud 2005 May 13 CME was chosen as a test case, with Wind/WAVES radiodata used to frame the inverse problem of finding the most likely progressionof burst locations. An MHD recreation is used to create synthetic spectra forvarious hypothesized burst locations. A framework is developed to score thesesynthetic spectra by their similarity to the type II frequency profile derivedfrom Wind/WAVES data. Simulated areas with 4x enhanced entropy and elevated deHoffmann Teller velocities are found to produce synthetic spectra similar tospacecraft observations. A geometrical analysis suggests that the eastern edgeof the entropy derived shock around (-30, 0) degrees in heliocentriccoordinates was emitting in the first hour of the event before ceasingemission, and that the western/southwestern edge of the shock centered around(6, -12) degrees was a dominant area of radio emission for the 2 hours ofsimulation data out to 20 solar radii.

Tracking the Source of Solar Type II Bursts through Comparisons of Simulations and Radio Data