Solar Radio Type-I Noise Storm Modulated by Coronal Mass Ejections

Details Solar Radio Type-I Noise Storm Modulated by Coronal Mass Ejections Solar Radio Type-I Noise Storm Modulated by Coronal Mass Ejections

Jan 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012apj...744..167i&link_type=abstract

The Astrophysical Journal, Volume 744, Issue 2, article id. 167 (2012).

Astronomy and Astrophysics

Astronomy

1

Sun: Corona, Sun: Coronal Mass Ejections: Cmes, Sun: Magnetic Topology, Sun: Radio Radiation

Scientific paper

The first coordinated observations of an active region using ground-based radio telescopes and the Solar Terrestrial Relations Observatory (STEREO) satellites from different heliocentric longitudes were performed to study solar radio type-I noise storms. A type-I noise storm was observed between 100 and 300 MHz during a period from 2010 February 6 to 7. During this period the two STEREO satellites were located approximately 65° (ahead) and -70° (behind) from the Sun-Earth line, which is well suited to observe the earthward propagating coronal mass ejections (CMEs). The radio flux of the type-I noise storm was enhanced after the preceding CME and began to decrease before the subsequent CME. This time variation of the type-I noise storm was directly related to the change of the particle acceleration processes around its source region. Potential-field source-surface extrapolation from the Solar and Heliospheric Observatory/Michelson Doppler Imager (SOHO/MDI) magnetograms suggested that there was a multipolar magnetic system around the active region from which the CMEs occurred around the magnetic neutral line of the system. From our observational results, we suggest that the type-I noise storm was activated at a side-lobe reconnection region that was formed after eruption of the preceding CME. This magnetic structure was deformed by a loop expansion that led to the subsequent CME, which then suppressed the radio burst emission.

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