Estimation of a Coronal Mass Ejection Magnetic Field Strength using Radio Observations of Gyrosynchrotron Radiation

Abstract

Coronal mass ejections (CMEs) are large eruptions of plasma and magnetic field from the low solar corona into interplanetary space. These eruptions are often associated with the acceleration of energetic electrons which produce various sources of high intensity plasma emission. In relatively rare cases, the energetic electrons may also produce gyrosynchrotron emission from within the CME itself, allowing for a diagnostic of the CME magnetic field strength. Such a magnetic field diagnostic is important for evaluating the total magnetic energy content of the CME, which is ultimately what drives the eruption. Here we report on an unusually large source of gyrosynchrotron radiation in the form of a type IV radio burst associated with a CME occurring on 2014-September-01, observed using instrumentation from the Nançay Radio Astronomy Facility. A combination of spectral flux density measurements from the Nançay instruments and the Radio Solar Telescope Network (RSTN) from 300MHz to 5 GHz reveals a gyrosynchrotron spectrum with a peak flux density at $>$1 GHz. Using this radio analysis, a model for gyrosynchrotron radiation, a non-thermal electron density diagnostic using the Fermi Gamma Ray Burst Monitor (GBM) and images of the eruption from the GOES Soft X-ray Imager (SXI), we are able to calculate both the magnetic field strength and the properties of the X-ray and radio emitting energetic electrons within the CME. We find the radio emission is produced by non-thermal electrons of energies >1MeV with a spectral index of $\delta$$\sim$3 in a CME magnetic field of 4.4 G at a height of 1.3 R${}_{\odot }$, while the X-ray emission is produced from a similar distribution of electrons but with much lower energies on the order of 10 keV. We conclude by comparing X-ray and radio-emitting electron distributions and how such an analysis can be used to define the plasma properties of a CME.

References in corpus (12)

• LOFAR: The LOw-Frequency ARray
• The Fermi Gamma-Ray Burst Monitor
• Global Energetics of Thirty-Eight Large Solar Eruptive Events
• The Relationship Between Solar Radio and Hard X-ray Emission
• Fermi-LAT Observations of High-energy Behind-the-limb Solar Flares
• Implications for electron acceleration and transport from non-thermal electron rates at looptop and footpoint sources in solar flares
• Observational evidence of torus instability as trigger mechanism for coronal mass ejections: the 2011 August 4 filament eruption
• An estimate of the magnetic field strength associated with a solar coronal mass ejection from low frequency radio observations
• On the variation of solar flare coronal x-ray source sizes with energy
• Origin of the 30 THz emission detected during the 2012 March 13 solar flare at 17:20 UT
• Coronal Mass Ejection Mass, Energy, and Force Estimates Using STEREO
• Solar Burst Analysis with 3D Loop Models

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