Magnetic Field Dynamics and Varying Plasma Emission in Large-scale Coronal Loops

Sahin, S.; Yurchyshyn, Vasyl; Kumar, Pankaj; Kılçık, Ali; Ahn, Kwangsu; Yang, Xu

doi:10.3847/1538-4357/ab04aa

Cited by 12 publications

(3 citation statements)

References 89 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Watanabe et al 2011;Vissers et al 2013;Peter et al 2014;Kim et al 2015;Vissers et al 2015;Rutten et al 2015;Rezaei & Beck 2015;Nelson et al 2016;Tian et al 2016;Reid et al 2016;Rutten 2016;Nelson et al 2017;Toriumi et al 2017;Hong et al 2017;Libbrecht et al 2017;van der Voort et al 2017;Tian et al 2018;Ulyanov et al 2019;Huang et al 2019;Chen et al 2019). In addition to the above energy bursts and plasma ejections, recent observations have suggested that the cancellation of opposite polarities at the footpoints of coronal loops could be responsible for the brightening of coronal loops (Tiwari et al 2014;Chitta et al 2017b;Huang et al 2018;Chitta et al 2018;Şahin et al 2019).…”

Section: Introductionmentioning

confidence: 99%

A Cancellation Nanoflare Model for Solar Chromospheric and Coronal Heating. III. 3D Simulations and Atmospheric Response

Syntelis

Priest

2020

ApJ

View full text Add to dashboard Cite

Inspired by recent observations suggesting that photospheric magnetic flux cancellation occurs much more frequently than previously thought, we analytically estimated the energy released from reconnection driven by photospheric flux cancellation, and proposed that it can act as a mechanism for chromospheric and coronal heating (Priest et al. 2018). Using two-dimensional simulations we validated the analytical estimates and studied the resulting atmospheric response (Syntelis et al. 2019). In the present work, we set up three-dimensional resistive MHD simulations of two cancelling polarities in a stratified atmosphere with a horizontal external field to further validate and improve upon the analytical estimates. The computational evaluation of the parameters associated with the energy release are in good qualitative agreement with the analytical estimates. The computational Poynting energy flux into the current sheet is in good qualitative agreement with the analytical estimates, after correcting the analytical expression to better account for the horizontal extent of the current sheet. The atmospheric response to the cancellation is the formation of hot ejections, cool ejections, or a combination of both hot and cool ejections, which can appear with a time difference and/or be spatially offset, depending on the properties of the cancelling region and the resulting height of the reconnection. Therefore, during the cancellation, a wide spectrum of ejections can be formed, which can account for the variety of multi-thermal ejections associated with Ellerman bombs, UV bursts and IRIS bombs, and also other ejections associated with small-scale cancelling regions and spicules.

show abstract

Section: Introductionmentioning

confidence: 99%

A Cancellation Nanoflare Model for Solar Chromospheric and Coronal Heating. III. 3D Simulations and Atmospheric Response

Syntelis

Priest

2020

ApJ

View full text Add to dashboard Cite

show abstract

“…Multiwavelength analysis is a widely used method in solar physics research. The community increasingly praises coordinated observations involving multiple instruments, allowing us to construct a comprehensive picture of a solar event (e.g., Ji et al 2012;Şahin et al 2019;Samanta et al 2019). Well-organized campaign observations among multiple space-and groundbased telescopes are playing an important role in solar physics studies.…”

Section: Introductionmentioning

confidence: 99%

GST Data-processing Workflow: Image Registration and Alignment

Yang

Cao

Yurchyshyn

2022

ApJS

Self Cite

View full text Add to dashboard Cite

Multiple solar instrument observation campaigns are increasingly popular among the solar physics and space science communities. Scientists organize high-resolution ground-based telescopes and spacecraft to study the evolution of the complex solar atmosphere and the origin of space weather. Image registration and coalignment between different instruments are vital for accurate data product comparison. We developed a Python language package for registration of ground-based high-resolution imaging data acquired by the Goode Solar Telescope (GST) to space-based full-disk continuum intensity data provided by the Solar Dynamics Observatory (SDO) with the scale-invariant feature transform method. The package also includes tools to align data sets obtained in different wavelengths and at different times utilizing the optical flow method. We present the image registration and coalignment workflow. The aliment accuracy of each alignment method is tested with the aid of radiative magnetohydrodynamics simulation data. We update the pointing information in GST data fits headers and generate GST and SDO imaging data products as science-ready four-dimensional (x, y, λ, t) data cubes.

show abstract

“…Aside from bursts and jets, observations have suggested that the cancellation of opposite polarities at the footpoints of coronal loops could be responsible for the brightening of coronal loops (Tiwari et al 2014;Chitta et al 2017Chitta et al , 2018Huang et al 2018;Şahin et al 2019). Potentially, even spicules could be linked to flux cancellation Samanta et al 2019).…”

Section: Introductionmentioning

confidence: 99%

Chromospheric and coronal heating and jet acceleration due to reconnection driven by flux cancellation

Syntelis

Priest

2021

A&A

View full text Add to dashboard Cite

Context. Recent observations have shown that magnetic flux cancellation occurs at the photosphere more frequently than previously thought. Aims. In order to understand the energy release by reconnection driven by flux cancellation, we previously studied a simple model of two cancelling polarities of equal flux. Here, we further develop our analysis to achieve a more general setup where the two cancelling polarities have unequal magnetic fluxes and where many new features are revealed. Methods. We carried out an analytical study of the cancellation of two magnetic fragments of unequal and opposite flux that approach one another and are located in an overlying horizontal magnetic field. Results. The energy release as microflares and nanoflares occurs in two main phases. During phase 1a, a separator is formed and reconnection is driven at it as it rises to a maximum height and then moves back down to the photosphere, heating the plasma and accelerating plasma jets in the process. During phase 1b, once the separator moves back to the photosphere, it bifurcates into two null points. Reconnection is no longer driven at the separator and an isolated magnetic domain connecting the two polarities is formed. During phase 2, the polarities cancel out at the photosphere as magnetic flux submerges below the photosphere and as reconnection occurs at and above the photosphere and plasma jets and a mini-filament eruption can be produced.

show abstract

Magnetic Field Dynamics and Varying Plasma Emission in Large-scale Coronal Loops

Cited by 12 publications

References 89 publications

A Cancellation Nanoflare Model for Solar Chromospheric and Coronal Heating. III. 3D Simulations and Atmospheric Response

A Cancellation Nanoflare Model for Solar Chromospheric and Coronal Heating. III. 3D Simulations and Atmospheric Response

GST Data-processing Workflow: Image Registration and Alignment

Chromospheric and coronal heating and jet acceleration due to reconnection driven by flux cancellation

Contact Info

Product

Resources

About