A 2D Model for Coronal Bright Points: Association with Spicules, UV bursts, Surges and EUV Coronal Jets

Abstract

Coronal Bright Points (CBPs) are ubiquitous structures in the solar atmosphere composed of hot small-scale loops observed in EUV or X-Rays in the quiet Sun and coronal holes. They are key elements to understand the heating of the corona; nonetheless, basic questions regarding their heating mechanisms, the chromosphere underneath, or the effects of flux emergence in these structures remain open. We have used the Bifrost code to carry out a 2D experiment in which a coronal-hole magnetic nullpoint configuration evolves perturbed by realistic granulation. To compare with observations, synthetic SDO/AIA, Solar Orbiter EUI-HRI, and IRIS images have been computed. The experiment shows the self-consistent creation of a CBP through the action of the stochastic granular motions alone, mediated by magnetic reconnection in the corona. The reconnection is intermittent and oscillatory, and it leads to coronal and transition-region temperature loops that are identifiable in our EUV/UV observables. During the CBP lifetime, convergence and cancellation at the surface of its underlying opposite polarities takes place. The chromosphere below the CBP shows a number of peculiar features concerning its density and the spicules in it. The final stage of the CBP is eruptive: magnetic flux emergence at the granular scale disrupts the CBP topology, leading to different ejections, such as UV bursts, surges, and EUV coronal jets. Apart from explaining observed CBP features, our results pave the way for further studies combining simulations and coordinated observations in different atmospheric layers.

arXiv commentAccepted in ApJL. 9 pages, 5 figures, 2 movies

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• High-resolution observations of recurrent jets from an arch filament system
• Deciphering the solar coronal heating: Energizing small-scale loops through surface convection
• A comparative study of resistivity models for simulations of magnetic reconnection in the solar atmosphere
• Small-scale magnetic flux emergence preceding a chain of energetic solar atmospheric events
• Thin coronal jets and plasmoid-mediated reconnection: Insights from Solar Orbiter observations and Bifrost simulations
• A comparative study of resistivity models for simulations of magnetic reconnection in the solar atmosphere. II. Plasmoid formation
• Magnetic Topology of quiet-Sun Ellerman bombs and associated Ultraviolet brightenings
• Extreme-ultraviolet (EUV) observables of simulated plasmoid-mediated reconnection in the solar corona
• Small-scale dynamic phenomena associated with interacting fan-spine topologies: quiet-Sun Ellerman bombs, UV brightenings, and chromospheric inverted-Y-shaped jets
• Differences in physical properties of coronal bright points and their ALMA counterparts within and outside coronal holes
• Resolving Interchange Reconnection Dynamics in a Fan-Spine-like Topology Observed by Solar Orbiter
• Observations of the formation of a proto-spot in a pre-existing field environment