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Eruptions from quiet Sun coronal bright points. I. Observations View all abstracts by submitter

Maria Madjarska   Submitted: 2018-08-15 12:35

Eruptions from coronal bright points (CBPs) are investigated in a two part study. The present study aims to explore in full detail the morphological and dynamical evolution of these eruptions in the context of the full lifetime evolution of CBPs. A follow-up study employs data-driven modelling based on a relaxation code to reproduce the time evolution of the magnetic field of these eruptive CBPs, and provide an insight on the possible causes for destabilisation and eruption. Observations of the full lifetime of CBPs in data taken with the AIA on board SDO in four passbands, He II 304 Å, Fe IX/X 171 Å, Fe XII 193 Å, and Fe XVIII 94 Å are investigated for the occurrence of plasma ejections, micro-flaring, mini-filament eruptions and mini coronal mass ejections (mini-CMEs). First and foremost, our study shows that the majority (76%) of quiet Sun CBPs (31 out of 42 CBPs) produce at least one eruption during their lifetime. From 21 eruptions in 11 CBPs, 18 occur in average ~17 hrs after the CBP formation for an average lifetime of the CBPs in AIA 193 Å of ~21 hrs. This time delay in the eruption occurrence coincides in each BP with the convergence and cancellation phase of the CBP bipole evolution during which the CBPs become smaller until they fully disappear. The remaining three happen 4 - 6 hrs after the CBP formation. In sixteen out of 21 eruptions the magnetic convergence and cancellation involve the CBP main bipoles, while in three eruptions one of the BP magnetic fragments and a pre-existing fragment of opposite polarity converge and cancel. In one BP with two eruptions cancellation was not observed. The CBP eruptions involve in most cases the expulsion of chromospheric material either as elongated filamentary structure (mini-filament, MF) or a volume of cool material (cool plasma cloud, CPC), together with the CBP or higher overlying hot loops. Coronal waves were identified during three eruptions. A micro-flaring is observed beneath all erupting MFs/CPCs. It remains uncertain whether the destabilised MF causes the micro-flaring or the destabilisation and eruption of the MF is triggered by reconnection beneath the filament. In most eruptions, the cool erupting plasma obscures partially or fully the micro-flare until the erupting material moves away from the CBP. From 21 eruptions 11 are found to produce mini-CMEs. The dimming regions associated with the CMEs are found to be occupied by both the "dark" cool plasma and areas of weakened coronal emission caused by the depleted plasma density. The present study demonstrates that the evolution of small-scale loop structures in the quiet Sun determined by their magnetic footpoint motions and/or ambient field topology, evolve into eruptive phase that triggers the ejection of cool and hot plasma in the corona

Authors: Chauzhou Mou, Maria S. Madjarska, Klaus Galsgaard, and Lidong Xia
Projects: SDO-AIA,SDO-HMI

Publication Status: in press in A&A
Last Modified: 2018-08-16 10:40
Go to main E-Print page  The Minimum Energy Principle Applied to Parker's Coronal Braiding and Nanoflaring Scenario  Evolution of the transverse density structure of oscillating coronal  loops inferred by forward modelling of EUV intensity  Edit Entry  Download Preprint  Delete Entry 

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