Bibcode
Matthews, Sarah A.; Williams, David R.; Klein, Karl-Ludwig; Kontar, Eduard P.; Smith, David M.; Lagg, Andreas; Krucker, Sam; Hurford, Gordon J.; Vilmer, Nicole; MacKinnon, Alexander L.; Zharkova, Valentina V.; Fletcher, Lyndsay; Hannah, Iain G.; Browning, Philippa K.; Innes, Davina E.; Trottet, Gerard; Foullon, Clare; Nakariakov, Valery M.; Green, Lucie M.; Lamoureux, Herve; Forsyth, Colin; Walton, David M.; Mathioudakis, Mihalis; Gandorfer, Achim; Martinez-Pillet, V.; Limousin, Olivier; Verwichte, Erwin; Dalla, Silvia; Mann, Gottfried; Aurass, Henri; Neukirch, Thomas
Referencia bibliográfica
Experimental Astronomy, Volume 33, Issue 2-3, pp. 237-269
Advertised on:
4
2012
Revista
Número de citas
3
Número de citas referidas
2
Descripción
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.
Proyectos relacionados
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Magnestismo Solar y Estelar
Los campos magnéticos son uno de los ingredientes fundamentales en la formación de estrellas y su evolución. En el nacimiento de una estrella, los campos magnéticos llegan a frenar su rotación durante el colapso de la nube molecular, y en el fin de la vida de una estrella, el magnetismo puede ser clave en la forma en la que se pierden las capas
Tobías
Felipe García
![Erupción de un filamento solar visto por AIA / SDO en el ultravioleta extremo. Imagen del Proyecto](/sites/default/files/styles/crop_square_2_2_to_320px/public/images/project/Imagen%20Tobias.jpg?itok=Ryks0yoA)
Magnestismo Solar y Estelar
Los campos magnéticos son uno de los ingredientes fundamentales en la formación de estrellas y su evolución. En el nacimiento de una estrella, los campos magnéticos llegan a frenar su rotación durante el colapso de la nube molecular, y en el fin de la vida de una estrella, el magnetismo puede ser clave en la forma en la que se pierden las capas
Tobías
Felipe García