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Tracking magnetic bright point motions through the solar atmosphere

Version 2 2024-06-05, 01:38
Version 1 2018-11-02, 15:08
journal contribution
posted on 2024-06-05, 01:38 authored by PH Keys, M Mathioudakis, DB Jess, Sergiy ShelyagSergiy Shelyag, DJ Christian, FP Keenan
High-cadence, multiwavelength observations and simulations are employed for the analysis of solar photospheric magnetic bright points (MBPs) in the quiet Sun. The observations were obtained with the Rapid Oscillations in the Solar Atmosphere (ROSA) imager and the Interferometric Bidimensional Spectrometer at the Dunn Solar Telescope. Our analysis reveals that photospheric MBPs have an average transverse velocity of approximately 1 kms-1, whereas their chromospheric counterparts have a slightly higher average velocity of 1.4 kms-1. Additionally, chromospheric MBPs were found to be around 63 per cent larger than the equivalent photospheric MBPs. These velocity values were compared with the output of numerical simulations generated using the MURAM code. The simulated results were similar, but slightly elevated, when compared to the observed data. An average velocity of 1.3 km s-1 was found in the simulated G-band images and an average of 1.8 km s-1 seen in the velocity domain at a height of 500 km above the continuum formation layer. Delays in the change of velocities were also analysed. Average delays of ~4 s between layers of the simulated data set were established and values of ~29 s observed between G-band and Ca II K ROSA observations. The delays in the simulations are likely to be the result of oblique granular shock waves, whereas those found in the observations are possibly the result of a semi-rigid flux tube.

History

Journal

Monthly notices of the Royal Astronomical Society

Volume

428

Pagination

3220-3226

Location

Oxford, Eng.

ISSN

0035-8711

eISSN

1365-2966

Language

eng

Publication classification

C1.1 Refereed article in a scholarly journal

Copyright notice

2012, The Authors

Issue

4

Publisher

Oxford University Press

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