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Solar Particle Acceleration Radiation and Kinetics (SPARK)

A mission to understand the nature of particle acceleration

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Abstract

Energetic particles are critical components of plasma populations found throughout the universe. In many cases particles are accelerated to relativistic energies and represent a substantial fraction of the total energy of the system, thus requiring extremely efficient acceleration processes. The production of accelerated particles also appears coupled to magnetic field evolution in astrophysical plasmas through the turbulent magnetic fields produced by diffusive shock acceleration. Particle acceleration is thus a key component in helping to understand the origin and evolution of magnetic structures in, e.g. galaxies. The proximity of the Sun and the range of high-resolution diagnostics available within the solar atmosphere offers unique opportunities to study the processes involved in particle acceleration through the use of a combination of remote sensing observations of the radiative signatures of accelerated particles, and of their plasma and magnetic environment. The SPARK concept targets the broad range of energy, spatial and temporal scales over which particle acceleration occurs in the solar atmosphere, in order to determine how and where energetic particles are accelerated. SPARK combines highly complementary imaging and spectroscopic observations of radiation from energetic electrons, protons and ions set in their plasma and magnetic context. The payload comprises focusing-optics X-ray imaging covering the range from 1 to 60 keV; indirect HXR imaging and spectroscopy from 5 to 200 keV, γ-ray spectroscopic imaging with high-resolution LaBr3 scintillators, and photometry and source localisation at far-infrared wavelengths. The plasma environment of the regions of acceleration and interaction will be probed using soft X-ray imaging of the corona and vector magnetography of the photosphere and chromosphere. SPARK is designed for solar research. However, in addition it will be able to provide exciting new insights into the origin of particle acceleration in other regimes, including terrestrial gamma-ray flashes (TGF), the origin of γ-ray bursts, and the possible existence of axions.

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Authors and Affiliations

  1. UCL Mullard Space Science Laboratory, Holmbury St. Mary, Dorking, RH5 6NT, UK

    Sarah A. Matthews, David R. Williams, Lucie M. Green, Herve Lamoureux, Colin Forsyth & David M. Walton

  2. LESIA, Observatoire de Paris-Meudon, Paris, France

    Karl-Ludwig Klein, Nicole Vilmer & Gerard Trottet

  3. SUPA, School of Physics & Astronomy, University of Glasgow, Glasgow, UK

    Eduard P. Kontar, Alexander L. MacKinnon, Lyndsay Fletcher & Iain G. Hannah

  4. UC Santa Cruz, Santa Cruz, CA, USA

    David M. Smith

  5. MPS, Lindau, Germany

    Andreas Lagg, Davina E. Innes & Achim Gandorfer

  6. UC Berkeley, Berkeley, CA, USA

    Sam Krucker

  7. University of Applied Sciences, North Western Switzerland (FHNW), Windisch, Switzerland

    Sam Krucker

  8. Space Sciences Lab. UC Berkeley, Berkeley, CA, USA

    Gordon J. Hurford

  9. University of Bradford, Bradford, UK

    Valentina V. Zharkova

  10. University of Manchester, Manchester, UK

    Philippa K. Browning

  11. University of Warwick, Conventry, UK

    Clare Foullon, Valery M. Nakariakov & Erwin Verwichte

  12. Queen’s University Belfast, Belfast, UK

    Mihalis Mathioudakis

  13. Instituto de Astrofisica de Canarias, La Laguna, Tenerife, Spain

    Valentin Martinez-Pillet

  14. CEA Saclay, Gif-sur-Yvette, France

    Olivier Limousin

  15. UCLan, Preston, UK

    Silvia Dalla

  16. AIP, Potsdam, Germany

    Gottfried Mann & Henri Aurass

  17. University of St. Andrews, St. Andrews, UK

    Thomas Neukirch

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Correspondence to Sarah A. Matthews.

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Matthews, S.A., Williams, D.R., Klein, KL. et al. Solar Particle Acceleration Radiation and Kinetics (SPARK). Exp Astron 33, 237–269 (2012). https://doi.org/10.1007/s10686-011-9260-3

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