Determining accurate plasma Doppler (line-of-sight) velocities from spectroscopic measurements is a challenging endeavour, especially when weak chromospheric absorption lines are often rapidly evolving and, hence, contain multiple spectral components in their constituent line profiles. Here, we present a novel method that employs machine learning techniques to identify the underlying components present within observed spectral lines, before subsequently constraining the constituent profiles through single or multiple Voigt fits. Our method allows active and quiescent components present in spectra to be identified and isolated for subsequent study. Lastly, we employ a Ca ii 8542 Å spectral imaging dataset as a proof-of-concept study to benchmark the suitability of our code for extracting two-component atmospheric profiles that are commonly present in sunspot chromospheres. Minimization tests are employed to validate the reliability of the results, achieving median reduced χ 2-values equal to 1.03 between the observed and synthesized umbral line profiles.
This article is part of the Theo Murphy meeting issue 'High-resolution wave dynamics in the lower solar atmosphere'.
|Number of pages||23|
|Journal||Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences|
|Early online date||21 Dec 2020|
|Publication status||Published - 08 Feb 2021|
Bibliographical noteFunding Information:
Data accessibility. The data used in this paper are from the observing campaign entitled ‘Nanoflare Activity in the Lower Solar Atmosphere’ (NSO-SP proposal T1020; principal investigator: DBJ), which employed the ground-based Dunn Solar Telescope, USA, during August 2014. The Dunn Solar Telescope at Sacramento Peak/NM was operated by the National Solar Observatory (NSO). NSO is operated by the Association of Universities for Research in Astronomy (AURA), Inc., under cooperative agreement with the National Science Foundation (NSF). Additional supporting observations were obtained from the publicly available NASA’s Solar Dynamics Observatory (https://sdo.gsfc.nasa.gov) data archive, which can be accessed via http://jsoc.stanford.edu/ajax/lookdata.html. The data that support the plots within this paper and other findings of this study are available from the corresponding author upon reasonable request. Authors’ contributions. C.D.M. and D.B.J. conceived of and designed the study. D.B.J. carried out the experiments. C.D.M. performed the data reduction and scientific analysis, with assistance from D.B.J., S.D.T.G., P.H.K. and M.S. C.D.M. drafted the manuscript, with theoretical input provided by E.K. All authors read and approved the manuscript. Competing interests. We declare we have no competing interests. Funding. This work was supported by The Department for the Economy (Northern Ireland) through their postgraduate research studentship and an Invest NI and Randox Laboratories Ltd. Research & Development (grant no. 059RDEN-1). Acknowledgements. C.D.M. would like to thank the Northern Ireland Department for the Economy for the award of a PhD studentship. D.B.J. and S.D.T.G. are grateful to Invest NI and Randox Laboratories Ltd. for the award of a Research & Development that allowed the computational techniques employed to be developed. The authors wish to acknowledge scientific discussions with the Waves in the Lower Solar Atmosphere (WaLSA; www.WaLSA.team) team, which is supported by the Research Council of Norway (project no. 262622), and The Royal Society through the award of funding to host the Theo Murphy Discussion Meeting ‘High-resolution wave dynamics in the lower solar atmosphere’ (grant no. Hooke18b/SCTM).
© 2020 The Author(s).
Copyright 2021 Elsevier B.V., All rights reserved.
- methods: Statistical
- Sun: Atmosphere
- Sun: Chromosphere
- Sun: Photosphere
- techniques: Spectroscopic
ASJC Scopus subject areas
- Physics and Astronomy(all)