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Coherent Synchrotron Radiation in Laboratory Accelerators and the Double-Spectral Feature in Solar Flares

Published online by Cambridge University Press:  12 September 2017

Wellington Cruz ,
Sérgio Szpigel ,
Pierre Kaufmann ,
Jean-Pierre Raulin  and
Michael Klopf
Wellington Cruz
Affiliation:
CRAAM, Mackenzie University, 01302-907, São Paulo, Brazil
Sérgio Szpigel
Affiliation:
CRAAM, Mackenzie University, 01302-907, São Paulo, Brazil
Pierre Kaufmann
Affiliation:
CRAAM, Mackenzie University, 01302-907, São Paulo, Brazil
Jean-Pierre Raulin
Affiliation:
CRAAM, Mackenzie University, 01302-907, São Paulo, Brazil
Michael Klopf
Affiliation:
Institute of Radiation Physics, Helmholtz-Zentrum, Dresden, Germany
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Abstract

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Recent observations of solar flares at high-frequencies have provided evidence of a new spectral component with fluxes increasing with frequency in the sub-THz to THz range. This new component occurs simultaneously but is separated from the well-known microwave spectral component that maximizes at frequencies of a few to tens of GHz. The aim of this work is to study in detail a mechanism recently suggested to describe the double-spectrum feature observed in solar flares based on the physical process known as microbunching instability, which occurs with high-energy electron beams in laboratory accelerators.

Keywords

Solar flaresCoherent synchrotron radiationMicrobunching instability
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S328: Living Around Active Stars , October 2016 , pp. 134 - 136
Copyright
Copyright © International Astronomical Union 2017 

References

Kaufmann, P. et al. 2002, Astrophys. J., v. 574, p. 1059–1065 CrossRefGoogle Scholar
Kaufmann, P. et al. 2004, Astrophys. J. Lett., v. 603, n. 2, p. L121 CrossRefGoogle Scholar
Silva, A. V. R. et al. 2007, Sol. Phys., v. 245, p. 311–326 CrossRefGoogle Scholar
Fernandes, L. O. T. et al. 2016, ASP Conf. Series, v. 504, p. 87 Google Scholar
Kaufmann, P. et al. 2013, Astrophys. J., v. 768, p. 134 CrossRefGoogle Scholar
Kaufmann, P. et al. 2015, J. Geophys. Res.: Space Phys., v. 120, n. 6, p. 4155–4163 CrossRefGoogle Scholar
Miteva, R. et al. 2016, Astron. Astrophys., v. 586, p. A91 CrossRefGoogle Scholar
Krucker, S. et al. 2016, Astron. Astrophys., v. 21:58 CrossRefGoogle Scholar
Kaufmann, P. & Raulin, J.-P. 2006, Phys. Plasmas, v. 13, 070701 CrossRefGoogle Scholar
Klopf, J. M., Kaufmann, P., & Raulin, J.-P. 2010, Bul. Am. Astron. Soc., v. 42, p. 905 Google Scholar
Klopf, J. M., Kaufmann, P., Raulin, J.-P., & Szpigel, S. 2014, Astrophy. J., v. 791, n. 1, p. 31 CrossRefGoogle Scholar
Friedman, M. & Herndon, M. 1973, Phys. of Fluids, v. 16, p. 1982–1995 CrossRefGoogle Scholar
Williams, G. P. 2002, Rev. Sci. Instr., v. 73, p. 1461–1463 CrossRefGoogle Scholar
Ingelman, G. & Siegbahn, K. 1998, Fysik-Aktuellt, v. 1, p. 3 Google Scholar