Observational signatures of a kink-unstable coronal flux rope using Hinode/EIS

Snow, Ben, Botha, Gert, Regnier, Stephane, Morton, Richard, Verwichte, Erwin and Young, Peter R. (2017) Observational signatures of a kink-unstable coronal flux rope using Hinode/EIS. The Astrophysical Journal, 842 (1). p. 16. ISSN 0004-637X

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Official URL: https://doi.org/10.3847/1538-4357/aa6d0e

Abstract

The signatures of energy release and energy transport for a kink-unstable coronal flux rope are investigated via forward modelling. 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 seconds. The synthetic images generated for rasters (moving slit) and sit-and-stare stationary slit) are analysed 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 towards 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).

Item Type: Article
Uncontrolled Keywords: magnetic reconnection; magnetohydrodynamics (MHD) ; Sun: corona; Sun: magnetic fields; Sun: UV radiation
Subjects: F300 Physics
F500 Astronomy
Department: Faculties > Engineering and Environment > Mathematics, Physics and Electrical Engineering
Depositing User: Ay Okpokam
Date Deposited: 11 May 2017 09:01
Last Modified: 28 Sep 2017 05:28
URI: http://nrl.northumbria.ac.uk/id/eprint/30435

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