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

Shetye, Juie, Shelyag, Sergiy, Reid, Aaron, Scullion, Eamon, Doyle, Jerry and Arber, Tony (2018) Signatures of the quiet Sun reconnection events in Ca II, Hα and Fe I. Monthly Notices of the Royal Astronomical Society, 479 (3). pp. 3274-3287. ISSN 0035-8711

[img]
Preview
Text
sty1548.pdf - Published Version
Available under License Creative Commons Attribution 4.0.

Download (9MB) | Preview
[img]
Preview
Text (Full text)
Shetye et al - Signatures of the quiet Sun reconnection events AAM.pdf - Accepted Version

Download (3MB) | Preview
Official URL: https://doi.org/10.1093/mnras/sty1548

Abstract

We use observations of quiet Sun (QS) regions in the Hα 6563 Å, Ca ii 8542 Å and Fe i 6302 Å lines. We observe brightenings in the wings of the Hα and Ca ii 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 which 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 (QSEBs) are formed at a higher height in the photosphere than the 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 Ca ii 8542 Å wing occurred before the peak in Hα wing. Moreover, in some cases, the line profiles observed in Ca ii are asymmetrical with a raised core profile. The source of heating in these events is shown by the MURaM simulations and is suggested to occur 430 km above the photosphere.

Item Type: Article
Uncontrolled Keywords: Sun: photosphere, Sun: chromosphere, Sun: magnetic fields, line: formation, line: profiles
Subjects: F300 Physics
F500 Astronomy
Department: Faculties > Engineering and Environment > Mathematics, Physics and Electrical Engineering
Depositing User: Paul Burns
Date Deposited: 04 Jun 2018 11:26
Last Modified: 11 Dec 2018 10:46
URI: http://nrl.northumbria.ac.uk/id/eprint/34463

Actions (login required)

View Item View Item

Downloads

Downloads per month over past year

View more statistics


Policies: NRL Policies | NRL University Deposit Policy | NRL Deposit Licence