|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|
|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).|
|Learning Resource Type||Article|
|Publisher Place||United States|
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