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Author Snow, B. ♦ Botha, G. J. J. ♦ Régnier, S. ♦ Morton, R. J. ♦ Young, P. R. ♦ Verwichte, E.
Source United States Department of Energy Office of Scientific and Technical Information
Content type Text
Language English
Subject Keyword ASTROPHYSICS, COSMOLOGY AND ASTRONOMY ♦ COMPUTERIZED SIMULATION ♦ EMISSION ♦ INSTABILITY ♦ MAGNETIC FIELDS ♦ MAGNETIC RECONNECTION ♦ MAGNETOHYDRODYNAMICS ♦ RESOLUTION ♦ SUN ♦ THREE-DIMENSIONAL CALCULATIONS ♦ ULTRAVIOLET RADIATION ♦ VELOCITY
Abstract The signatures of energy release and energy transport for a kink-unstable coronal flux rope are investigated via forward modeling. Synthetic intensity and Doppler maps are generated from a 3D numerical simulation. The CHIANTI database is used to compute intensities for three Hinode /EIS emission lines that cover the thermal range of the loop. The intensities and Doppler velocities at simulation-resolution are spatially degraded to the Hinode /EIS pixel size (1″), convolved using a Gaussian point-spread function (3″), and exposed for a characteristic time of 50 s. The synthetic images generated for rasters (moving slit) and sit-and-stare (stationary slit) are analyzed to find the signatures of the twisted flux and the associated instability. We find that there are several qualities of a kink-unstable coronal flux rope that can be detected observationally using Hinode /EIS, namely the growth of the loop radius, the increase in intensity toward the radial edge of the loop, and the Doppler velocity following an internal twisted magnetic field line. However, EIS cannot resolve the small, transient features present in the simulation, such as sites of small-scale reconnection (e.g., nanoflares).
ISSN 0004637X
Educational Use Research
Learning Resource Type Article
Publisher Date 2017-06-10
Publisher Place United States
Journal Astrophysical Journal
Volume Number 842
Issue Number 1


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