E-Print Archive

There are 3969 abstracts currently viewable.


Advanced Search
Main Page Add New E-Print Submitter
News Help/FAQ About Preferences
Manage Key Phrase
Estimation of a Coronal Mass Ejection Magnetic Field Strength using Radio Observations of Gyrosynchrotron Radiation View all abstracts by submitter

Eoin Carley   Submitted: 2017-09-18 04:01

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 300 MHz 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 δ∼3 in a CME magnetic field of 4.4 G at a height of 1.3 R⊙, 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 the electron distribution characteristics derived from both X-ray and radio and show how such an analysis can be used to define the plasma and bulk properties of a CME.

Authors: Eoin P. Carley, Nicole Vilmer, Paulo J. A. Simões, Brían Ó Fearraigh
Projects: None

Publication Status: In press
Last Modified: 2017-09-20 09:04
Go to main E-Print page  Energy release in the solar atmosphere from a stream of infalling prominence debris  QUASI-PERIODIC OSCILLATIONS IN FLARES AND CORONAL MASS EJECTIONS ASSOCIATED WITH MAGNETIC RECONNECTION  Edit Entry  Download Preprint  Submitter's Homepage Delete Entry 

Go to main E-Print pageGo to main E-Print page.
Previous AbstractPrevious Abstract.
Next AbstractNext Abstract.
Download PreprintDownload Preprint.
Submitter's HomepageSubmitters Homepage.
Edit EntryEdit Entry.
View All Abstracts By SubmitterView all abstracts by submitter.
Delete AbstractDelete abstract.

Latest Entries
CME-driven shock and Type II solar radio burst band-splitting
Signatures of magnetic reconnection at the footpoints of fan shape jets on a light bridge driven by photospheric convective motions
Drifting of the line-tied footpoints of CME flux-ropes
Three-dimensional Magnetic Reconnection Triggering an X-class Confined Flare in Active Region 12192
Oscillations accompanying a He I 10830 Å negative flare in a solar facula
The Origin of Major Solar Activity - Collisional Shearing Between Nonconjugated Polarities of Multiple Bipoles Emerging Within Active Regions
Probing the Puzzle of Behind-the-limb γ-Ray Flares: Data-driven Simulations of Magnetic Connectivity and CME-driven Shock Evolution
Transition-region explosive events produced by plasmoid instability
Flare Productivity of Major Flaring Solar Active Regions: A Time-series Study of Photospheric Magnetic Properties
Physical processes involved in the EUV "Surge" Event of 09 May 2012
Formation and Eruption of an Active Region Sigmoid. II. Magnetohydrodynamic Simulation of a Multistage Eruption
Evolution of Photospheric Vector Magnetic Field Associated with Moving Flare Ribbons As Seen By GST
On the Extrapolation of Magnetohydrostatic Equilibria on the Sun
Lyman Continuum Observations of Solar Flares Using SDO/EVE
Buoyancy-driven Magnetohydrodynamic Waves in a Partially Ionized Plasma
Genesis and impulsive evolution of the 2017 September 10 coronal mass ejection
First Detection of Solar Flare Emission in Middle-Ultraviolet Balmer Continuum
First high-resolution look at the quiet Sun with ALMA at 3 mm
Dispersive shock waves in partially ionised plasmas
Frequency rising sub-THz emission from solar flare ribbons

Related Pages
MSU Solar Physics.
Max Millennium Science Mail Archive.
Max Millennium Message of the Day Mail Archive.
Max Millennium Flare Catalog

Archive Maintainer
Alisdair Davey

© 2003 Solar Physics Group - Montana State University