Imaging and Spectroscopy of Six NuSTAR MicroFlares SH11D-2898 Contact: J. Duncan1, L. Glesener1, I. Hannah2, D. Smith3, B. Grefenstette4 (1Univ, of Minnesota; 2Univ. of Glasgow; 3UC Santa Cruz; 4California Institute of Technology)
[email protected] Abstract MicroFlare Time Evolution Hard X-ray (HXR) emission in solar flares originates from regions of high temperature plasma, as well as from non-thermal particle populations [1]. Both of these sources of HXR radiation make solar observation in this band important for study of • NuSTAR observed 6 MicroFlares during this observation. Time evolution is shown in both raw and normalized NuSTAR flare energetics. NuSTAR is the first HXR telescope with direct focusing optics, giving it a dramatic increase in sensitivity countsLivetime acrosscorrection several applied energy ranges for each flare. Counts are livetime-corrected (NuSTAR livetime ranged from 1-14%). Livetime correction applied over previous indirect imaging methods. Here we present NuSTAR observation of six microflares from one solar active Livetime correction applied 5 5 6 5×10 4×10 2.0 10 5 × 4×10 5 region during a period of several hours on May 29th, 2018. In conjunction with simultaneous data from SDO/AIA, data 3×10 5 2-4 keV 2-4 keV 6 3×10 1.5 10 Orbit1, Flare B 4-6 keV 2×105 4-6 keV × 5 counts 2 10 2-4 keV × Orbit1, Flare A 6-8 keV counts Orbit1, Flare C 6-8 keV from this observation has been used to create flare-time images showing the spatial extent of HXR emission. Additionally, 5 5 1 10 1×10 8-10 keV × 8-10 keV 6 4-6 keV 1.0×10 (Left) Estimated GOES A5 flare, with 0 0 1.2 1.2 16:07 16:08 16:09 16:10 16:11 16:46 16:48 16:50 16:52 16:54 NuSTAR lightcurves show time evolution in four different HXR energy ranges over the course of each flare.