Origin of the Submillimeter Radio Emission During the Time-Extended Phase of a Solar Flare

@article{Trottet2011OriginOT,
  title={Origin of the Submillimeter Radio Emission During the Time-Extended Phase of a Solar Flare},
  author={G{\'e}rard Trottet and Jean Pierre Raulin and G. Gim{\'e}nez de Castro and Thomas L{\"u}thi and Amir Caspi and Cristina H. Mandrini and Mar{\'i}a Luisa Luoni and Pierre Kaufmann},
  journal={Solar Physics},
  year={2011},
  volume={273},
  pages={339-361}
}
Solar flares observed in the 200 – 400 GHz radio domain may exhibit a slowly varying and time-extended component which follows a short (few minutes) impulsive phase and can last for a few tens of minutes to more than one hour. The few examples discussed in the literature indicate that such long-lasting submillimeter emission is most likely thermal bremsstrahlung. We present a detailed analysis of the time-extended phase of the 27 October 2003 (M6.7) flare, combining 1 – 345 GHz total-flux radio… 

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References

SHOWING 1-10 OF 45 REFERENCES

Analysis of the impulsive phase of a solar flare at submillimeter wavelengths

We present a report on the strong X5.3 solar flare which occurred on 25 August 2001, producing high-level γ-ray activity, nuclear lines and a dramatic long-duration white-light continuum. The bulk of

Submillimeter and X-ray observations of an X class flare

The GOES X1.5 class flare that occurred on August 30, 2002 at 1327:30 UT is one of the few events detected so far at submillimeter wavelengths. We present a detailed analysis of this flare combining

First detection of the impulsive and extended phases of a solar radio burst above 200 GHz

We present a detailed analysis of radio observations obtained at 212 and 405 GHz during the 2000 March 22 H α 2N flare that occured in AR8910 at ~1834 UT. These data are compared with microwave, soft

First observation of a solar X-class flare in the submillimeter range with KOSMA

We present the first solar flare observations with the KOSMA submillimeter telescope at 230 and 345 GHz. The GOES X2.0 flare on April 12, 2001 was also observed at millimeter and centimeter

Radio Submillimeter and γ-Ray Observations of the 2003 October 28 Solar Flare

Radio observations at 210 GHz taken by the Bernese Multibeam Radiometer for KOSMA (BEMRAK) are combined with hard X-ray and γ-ray observations from the SONG instrument on board CORONA-F and the

A New Solar Burst Spectral Component Emitting Only in the Terahertz Range

Solar flare energy manifestations were believed to be the result of the same kind of particle acceleration. It is generally accepted that a population of relativistic electrons accelerated during the

Determination of the location and effective angular size of solar flares with a 210 GHz multibeam radiometer

We report on the study and successful application of an improved measurement method for solar flares at millimeter wavelengths. A 210 GHz multibeam receiver for the observation of solar bursts was

Evidence that Synchrotron Emission from Nonthermal Electrons Produces the Increasing Submillimeter Spectral Component in Solar Flares

Abstract We investigate the origin of the increasing spectra observed at submillimeter wavelengths detected in the flare on 2 November 2003 starting at 17:17 UT. This flare, classified as an X8.3 and

Multiple Components in the Millimeter Emission of a Solar Flare

We analyze a small flare using imaging data at millimeter, microwave, and soft X-ray wavelengths and microwave and hard X-ray spectral observations. The remarkable aspect of this flare is evidence

RHESSI LINE AND CONTINUUM OBSERVATIONS OF SUPER-HOT FLARE PLASMA

We use RHESSI high-resolution imaging and spectroscopy observations from ∼5 to 100 keV to characterize the hot thermal plasma during the 2002 July 23 X4.8 flare. These measurements of the steeply