Authors: Surajit Mondal (NJIT), Bin Chen (NJIT), Dale E. Gary (NJIT), Gregg Hallinan (CALTECH), Marin Anderson (JPL), Ivey Davis (CALTECH), Brian O’Donnell (NJIT), Sherry Chhabra (GMU), Casey Law (CALTECH), Yuping Huang (CALTECH), and the OVRO-LWA Team

Coronal Mass Ejections (CMEs) play a very important role in space weather. Out of all the properties which determine the geo-effectiveness of CMEs, the magnetic field is perhaps the least constrained one. Radio observations can play a significant role in providing this crucial information. Detection and modeling of the CME gyrosynchrotron emission can be used to constrain the CME magnetic field. Observations with the Nancay Radioheliograph, Murchison Widefield Array and the newly introduced solar-dedicated Owens Valley Long Wavelength Array (OVRO-LWA; under commissioning) show that it is possible to detect the radio emission from CMEs. Here we shall present some results from the MWA to show how we can use the radio and optical data to make a spatially resolved map of the CME magnetic field. We will also present some preliminary results using data from the OVRO-LWA, which is planned to include a solar-dedicated mode to demonstrate that it might indeed be possible to detect the CME radio emission rather routinely. This opens up the exciting possibility of not only measuring the spatially resolved magnetic field in radio-emitting CMEs, but to track its evolution as well.