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Solar Physics

, Volume 255, Issue 1, pp 131–142 | Cite as

Sub-terahertz, Microwaves and High Energy Emissions During the 6 December 2006 Flare, at 18:40 UT

  • Pierre Kaufmann
  • Gérard Trottet
  • C. Guillermo Giménez de Castro
  • Jean-Pierre Raulin
  • Säm Krucker
  • Albert Y. Shih
  • Hugo Levato
Article

Abstract

The presence of a solar burst spectral component with flux density increasing with frequency in the sub-terahertz range, spectrally separated from the well-known microwave spectral component, bring new possibilities to explore the flaring physical processes, both observational and theoretical. The solar event of 6 December 2006, starting at about 18:30 UT, exhibited a particularly well-defined double spectral structure, with the sub-THz spectral component detected at 212 and 405 GHz by the Solar Submilimeter Telescope (SST) and microwaves (1 – 18 GHz) observed by the Owens Valley Solar Array (OVSA). Emissions obtained by instruments onboard satellites are discussed with emphasis to ultra-violet (UV) obtained by the Transition Region And Coronal Explorer (TRACE), soft X-rays from the Geostationary Operational Environmental Satellites (GOES) and X- and γ-rays from the Ramaty High Energy Solar Spectroscopic Imager (RHESSI). The sub-THz impulsive component had its closer temporal counterparts only in the higher energy X- and γ-rays ranges. The spatial positions of the centers of emission at 212 GHz for the first flux enhancement were clearly displaced by more than one arc-minute from positions at the following phases. The observed sub-THz fluxes and burst source plasma parameters were difficult to be reconciled with a purely thermal emission component. We discuss possible mechanisms to explain the double spectral components at microwaves and in the THz ranges.

Keywords

Solar Phys Spectral Component Turnover Frequency Impulsive Phase Ramaty High Energy Solar Spectroscopic Imager 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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Copyright information

© Springer Science+Business Media B.V. 2009

Authors and Affiliations

  • Pierre Kaufmann
    • 1
    • 2
  • Gérard Trottet
    • 3
  • C. Guillermo Giménez de Castro
    • 1
  • Jean-Pierre Raulin
    • 1
  • Säm Krucker
    • 4
  • Albert Y. Shih
    • 4
  • Hugo Levato
    • 5
  1. 1.Centro de Rádio-Astronomia e Astrofísica Mackenzie, Escola de EngenhariaUniversidade Presbiteriana MackenzieSão PauloBrazil
  2. 2.Centro de Componentes SemicondutoresUniversidade Estadual de CampinasCampinasBrazil
  3. 3.LESIAObservatoire de Paris-MeudonMeudonFrance
  4. 4.Space Sciences LaboratoryUniversity of California BerkeleyBerkeleyUSA
  5. 5.Complejo Astronómico El LeoncitoSan JuanArgentina

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