Solar filaments exist as stable structures for extended periods of time before many of them form the core of a coronal mass ejection (CME). We examine the properties of an erupting filament on 2017 May 29–30 with high-resolution He
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Abstract i 10830 Å and Hα spectra from the Dunn Solar Telescope, full-disk Dopplergrams of Hei 10830 Å from the Chromospheric Telescope, and EUV and coronograph data from SDO and STEREO. Pre-eruption line-of-sight velocities from an inversion of Hei with the HAZEL code exhibit coherent patches of 5 Mm extent that indicate counter-streaming and/or buoyant behavior. During the eruption, individual, aligned threads appear in the Hei velocity maps. The distribution of velocities evolves from Gaussian to strongly asymmetric. The maximal optical depth of Hei 10830 Å decreased fromτ = 1.75 to 0.25, the temperature increased by 13 kK, and the average speed and width of the filament increased from 0 to 25 km s−1and 10 to 20 Mm, respectively. All data sources agree that the filament rose with an exponential acceleration reaching 7.4 m s−2that increased to a final velocity of 430 km s−1at 22:24 UT; a CME was associated with this filament eruption. The properties during the eruption favor a kink/torus instability, which requires the existence of a flux rope. We conclude that full-disk chromospheric Dopplergrams can be used to trace the initial phase of on-disk filament eruptions in real time, which might potentially be useful for modeling the source of any subsequent CMEs. -
Wang, Shuo ; Jenkins, Jack M. ; Martinez Pillet, Valentin ; Beck, Christian ; Long, David M. ; Prasad Choudhary, Debi ; Muglach, Karin ; McAteer, James ( , The Astrophysical Journal)