Signatures of quiet Sun reconnection events in Ca II, Hα, and Fe I

Shetye, J, Shelyag, Sergiy, Reid, AL, Scullion, E, Doyle, JG and Arber, TD 2018, Signatures of quiet Sun reconnection events in Ca II, Hα, and Fe I, Monthly notices of the Royal Astronomical Society, vol. 479, no. 3, pp. 3274-3287, doi: 10.1093/mnras/sty1548.

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Title Signatures of quiet Sun reconnection events in Ca II, Hα, and Fe I
Author(s) Shetye, J
Shelyag, SergiyORCID iD for Shelyag, Sergiy orcid.org/0000-0002-6436-9347
Reid, AL
Scullion, E
Doyle, JG
Arber, TD
Journal name Monthly notices of the Royal Astronomical Society
Volume number 479
Issue number 3
Start page 3274
End page 3287
Total pages 14
Publisher Oxford University Press
Place of publication Oxford, Eng.
Publication date 2018-09
ISSN 0035-8711
1365-2966
Keyword(s) formation
profiles
Sun: chromosphere
Sun: photosphere
science & technology
physical sciences
astronomy & astrophysics
Summary We use observations of quiet Sun (QS) regions in the Hα 6563 Å, CaII 8542 Å, and FeI 6302 Å lines. We observe brightenings in the wings of the Hα and CaII combined with observations of the interacting magnetic concentrations observed in the Stokes signals of Fe I. These brightenings are similar to Ellerman bombs (EBs), i.e. impulsive bursts in the wings of the Balmer lines that leave the line cores unaffected. Such enhancements suggest that these events have similar formation mechanisms to the classical EBs found in active regions, with the reduced intensity enhancements found in the QS regions due to a weaker feeding magnetic flux. The observations also show that the quiet Sun Ellerman bombs are formed at a higher height in the upper photosphere than the photospheric continuum level. Using simulations, we investigate the formation mechanism associated with the events and suggest that these events are driven by the interaction of magnetic field lines in the upper photospheric regions. The results of the simulation are in agreement with observations when comparing the light curves, and in most cases, we found that the peak in the CaII 8542 Å wing occurred before the peak in Hα wing. Moreover, in some cases, the line profiles observed in CaII are asymmetrical with a raised core profile. The source of heating in these events is shown by theMURaM simulations and is suggested to occur 430 km above the photosphere.
Language eng
DOI 10.1093/mnras/sty1548
Field of Research 0201 Astronomical And Space Sciences
HERDC Research category C1.1 Refereed article in a scholarly journal
Copyright notice ©2018, The Author(s)
Persistent URL http://hdl.handle.net/10536/DRO/DU:30114935

Document type: Journal Article
Collection: School of Information Technology
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