Magnetoacoustic wave energy dissipation in the atmosphere of solar pores

Caitlin A. Gilchrist-Millar; David B. Jess; Samuel D.T. Grant; Peter H. Keys; Christian Beck; Shahin Jafarzadeh; Julia M. Riedl; Tom Van Doorsselaere; Basilio Ruiz Cobo

doi:10.1098/rsta.2020.0172

Magnetoacoustic wave energy dissipation in the atmosphere of solar pores

Caitlin A. Gilchrist-Millar^*, David B. Jess, Samuel D.T. Grant, Peter H. Keys, Christian Beck, Shahin Jafarzadeh, Julia M. Riedl, Tom Van Doorsselaere, Basilio Ruiz Cobo

^*Corresponding author for this work

Research output: Contribution to journal › Article › peer-review

25 Citations (Scopus)

Abstract

The suitability of solar pores as magnetic wave guides has been a key topic of discussion in recent years. Here, we present observational evidence of propagating magnetohydrodynamic wave activity in a group of five photospheric solar pores. Employing data obtained by the Facility Infrared Spectropolarimeter at the Dunn Solar Telescope, oscillations with periods of the order of 5 min were detected at varying atmospheric heights by examining Si 10827 Å line bisector velocities. Spectropolarimetric inversions, coupled with the spatially resolved root mean square bisector velocities, allowed the wave energy fluxes to be estimated as a function of atmospheric height for each pore. We find propagating magnetoacoustic sausage mode waves with energy fluxes on the order of 30kWm-2 at an atmospheric height of 100 km, dropping to approximately 2kWm-2 at an atmospheric height of around 500 km. The cross-sectional structuring of the energy fluxes reveals the presence of both body- A nd surface-mode sausage waves. Examination of the energy flux decay with atmospheric height provides an estimate of the damping length, found to have an average value across all five pores of L d ≈ 268km, similar to the photospheric density scale height. We find the damping lengths are longer for body mode waves, suggesting that surface mode sausage oscillations are able to more readily dissipate their embedded wave energies. This work verifies the suitability of solar pores to act as efficient conduits when guiding magnetoacoustic wave energy upwards into the outer solar atmosphere. This article is part of the Theo Murphy meeting issue 'High-resolution wave dynamics in the lower solar atmosphere'.

Original language	English
Article number	20200172
Number of pages	19
Journal	Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences
Volume	379
Issue number	2190
Early online date	21 Dec 2020
DOIs	https://doi.org/10.1098/rsta.2020.0172
Publication status	Published - 08 Feb 2021

Bibliographical note

Funding Information:
Data accessibility. The data used in this paper are from the observing campaign entitled ‘The Influence of Magnetism on Solar and Stellar Atmospheric Dynamics’ (NSO-SP proposal T1081; principal investigator: D.B.J.), which employed the ground-based Dunn Solar Telescope, USA, during July 2016. 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.

Funding Information:
Authors’ contributions. D.B.J. carried out the experiments and conceived of and designed the study. C.A.G.-M. performed the data reduction and scientific analysis, with assistance from D.B.J., S.D.T.G., P.H.K., C.B., S.J. and B.R.C. C.A.G.-M. drafted the manuscript, with theoretical input provided by J.M.R. and T.V.D. All authors read and approved the manuscript. Competing interests. We declare we have no competing interests. Funding. This study was supported by Invest NI and Randox Laboratories Ltd. Research & Development Grant (059RDEN-1); European Union’s Horizon 2020 research and innovation programme (grant agreement no. 682462); Research Council of Norway through its Centres of Excellence scheme (project no. 262622); European Union’s Horizon 2020 research and innovation programme (grant agreement no. 724326); Research Council of Norway (project no. 262622) and The Royal Society (grant no. Hooke18b/SCTM). Acknowledgements. C.A.G.-M., D.B.J. and S.D.T.G. are grateful to Invest NI and Randox Laboratories Ltd. for the award of a Research & Development Grant (059RDEN-1) that allowed the computational techniques employed to be developed. S.J. acknowledges support from the European Research Council under the European Union’s Horizon 2020 research and innovation programme (grant agreement no. 682462) and from the Research Council of Norway through its Centres of Excellence scheme (project no. 262622). J.M.R. and T.V.D. were supported by the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No 724326). T.V.D. received further support from the C1 grant TRACEspace of Internal Funds KU Leuven (number C14/19/089). The space-based data employed in this work is courtesy of NASA/SDO and the AIA, EVE and HMI science teams. 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 number 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 Hooke18b/SCTM).

Publisher Copyright:
© 2020 The Author(s).

Copyright:
Copyright 2021 Elsevier B.V., All rights reserved.

Keywords

Sun: Atmosphere
Sun: Magnetic fields
Sun: Oscillations
Sun: Photosphere
sunspots
techniques: Polarimetric

ASJC Scopus subject areas

General Mathematics
General Engineering
General Physics and Astronomy

Access to Document

10.1098/rsta.2020.0172Licence: Unspecified

Magnetoacoustic Wave Energy Dissipation in the Atmosphere of Solar Pores
Gilchrist-Millar, C. (Presenter)
13 Nov 2020
Activity: Talk or presentation types › Oral presentation

Magnetoacoustic wave dynamics in the atmosphere of solar active regions
Gilchrist-Millar, C. (Author), Jess, D. (Supervisor), Grant, S. (Supervisor) & Mathioudakis, M. (Supervisor), Dec 2022
Student thesis: Doctoral Thesis › Doctor of Philosophy

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Gilchrist-Millar, C. A., Jess, D. B., Grant, S. D. T., Keys, P. H., Beck, C., Jafarzadeh, S., Riedl, J. M., Van Doorsselaere, T., & Ruiz Cobo, B. (2021). Magnetoacoustic wave energy dissipation in the atmosphere of solar pores. Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences, 379(2190), Article 20200172. https://doi.org/10.1098/rsta.2020.0172

@article{66593f564ea741deb12f65a6bd999556,

title = "Magnetoacoustic wave energy dissipation in the atmosphere of solar pores",

abstract = "The suitability of solar pores as magnetic wave guides has been a key topic of discussion in recent years. Here, we present observational evidence of propagating magnetohydrodynamic wave activity in a group of five photospheric solar pores. Employing data obtained by the Facility Infrared Spectropolarimeter at the Dunn Solar Telescope, oscillations with periods of the order of 5 min were detected at varying atmospheric heights by examining Si 10827 {\AA} line bisector velocities. Spectropolarimetric inversions, coupled with the spatially resolved root mean square bisector velocities, allowed the wave energy fluxes to be estimated as a function of atmospheric height for each pore. We find propagating magnetoacoustic sausage mode waves with energy fluxes on the order of 30kWm-2 at an atmospheric height of 100 km, dropping to approximately 2kWm-2 at an atmospheric height of around 500 km. The cross-sectional structuring of the energy fluxes reveals the presence of both body- A nd surface-mode sausage waves. Examination of the energy flux decay with atmospheric height provides an estimate of the damping length, found to have an average value across all five pores of L d ≈ 268km, similar to the photospheric density scale height. We find the damping lengths are longer for body mode waves, suggesting that surface mode sausage oscillations are able to more readily dissipate their embedded wave energies. This work verifies the suitability of solar pores to act as efficient conduits when guiding magnetoacoustic wave energy upwards into the outer solar atmosphere. This article is part of the Theo Murphy meeting issue 'High-resolution wave dynamics in the lower solar atmosphere'. ",

keywords = "Sun: Atmosphere, Sun: Magnetic fields, Sun: Oscillations, Sun: Photosphere, sunspots, techniques: Polarimetric",

author = "Gilchrist-Millar, {Caitlin A.} and Jess, {David B.} and Grant, {Samuel D.T.} and Keys, {Peter H.} and Christian Beck and Shahin Jafarzadeh and Riedl, {Julia M.} and {Van Doorsselaere}, Tom and {Ruiz Cobo}, Basilio",

note = "Funding Information: Data accessibility. The data used in this paper are from the observing campaign entitled {\textquoteleft}The Influence of Magnetism on Solar and Stellar Atmospheric Dynamics{\textquoteright} (NSO-SP proposal T1081; principal investigator: D.B.J.), which employed the ground-based Dunn Solar Telescope, USA, during July 2016. 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{\textquoteright}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. Funding Information: Authors{\textquoteright} contributions. D.B.J. carried out the experiments and conceived of and designed the study. C.A.G.-M. performed the data reduction and scientific analysis, with assistance from D.B.J., S.D.T.G., P.H.K., C.B., S.J. and B.R.C. C.A.G.-M. drafted the manuscript, with theoretical input provided by J.M.R. and T.V.D. All authors read and approved the manuscript. Competing interests. We declare we have no competing interests. Funding. This study was supported by Invest NI and Randox Laboratories Ltd. Research & Development Grant (059RDEN-1); European Union{\textquoteright}s Horizon 2020 research and innovation programme (grant agreement no. 682462); Research Council of Norway through its Centres of Excellence scheme (project no. 262622); European Union{\textquoteright}s Horizon 2020 research and innovation programme (grant agreement no. 724326); Research Council of Norway (project no. 262622) and The Royal Society (grant no. Hooke18b/SCTM). Acknowledgements. C.A.G.-M., D.B.J. and S.D.T.G. are grateful to Invest NI and Randox Laboratories Ltd. for the award of a Research & Development Grant (059RDEN-1) that allowed the computational techniques employed to be developed. S.J. acknowledges support from the European Research Council under the European Union{\textquoteright}s Horizon 2020 research and innovation programme (grant agreement no. 682462) and from the Research Council of Norway through its Centres of Excellence scheme (project no. 262622). J.M.R. and T.V.D. were supported by the European Research Council (ERC) under the European Union{\textquoteright}s Horizon 2020 research and innovation programme (grant agreement No 724326). T.V.D. received further support from the C1 grant TRACEspace of Internal Funds KU Leuven (number C14/19/089). The space-based data employed in this work is courtesy of NASA/SDO and the AIA, EVE and HMI science teams. 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 number 262622), and The Royal Society through the award of funding to host the Theo Murphy Discussion Meeting {\textquoteleft}High resolution wave dynamics in the lower solar atmosphere{\textquoteright} (grant Hooke18b/SCTM). Publisher Copyright: {\textcopyright} 2020 The Author(s). Copyright: Copyright 2021 Elsevier B.V., All rights reserved.",

year = "2021",

month = feb,

day = "8",

doi = "10.1098/rsta.2020.0172",

language = "English",

volume = "379",

journal = "Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences",

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Gilchrist-Millar, CA, Jess, DB , Grant, SDT , Keys, PH, Beck, C, Jafarzadeh, S, Riedl, JM, Van Doorsselaere, T & Ruiz Cobo, B 2021, 'Magnetoacoustic wave energy dissipation in the atmosphere of solar pores', Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences, vol. 379, no. 2190, 20200172. https://doi.org/10.1098/rsta.2020.0172

TY - JOUR

T1 - Magnetoacoustic wave energy dissipation in the atmosphere of solar pores

AU - Gilchrist-Millar, Caitlin A.

AU - Jess, David B.

AU - Grant, Samuel D.T.

AU - Keys, Peter H.

AU - Beck, Christian

AU - Jafarzadeh, Shahin

AU - Riedl, Julia M.

AU - Van Doorsselaere, Tom

AU - Ruiz Cobo, Basilio

N1 - Funding Information: Data accessibility. The data used in this paper are from the observing campaign entitled ‘The Influence of Magnetism on Solar and Stellar Atmospheric Dynamics’ (NSO-SP proposal T1081; principal investigator: D.B.J.), which employed the ground-based Dunn Solar Telescope, USA, during July 2016. 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. Funding Information: Authors’ contributions. D.B.J. carried out the experiments and conceived of and designed the study. C.A.G.-M. performed the data reduction and scientific analysis, with assistance from D.B.J., S.D.T.G., P.H.K., C.B., S.J. and B.R.C. C.A.G.-M. drafted the manuscript, with theoretical input provided by J.M.R. and T.V.D. All authors read and approved the manuscript. Competing interests. We declare we have no competing interests. Funding. This study was supported by Invest NI and Randox Laboratories Ltd. Research & Development Grant (059RDEN-1); European Union’s Horizon 2020 research and innovation programme (grant agreement no. 682462); Research Council of Norway through its Centres of Excellence scheme (project no. 262622); European Union’s Horizon 2020 research and innovation programme (grant agreement no. 724326); Research Council of Norway (project no. 262622) and The Royal Society (grant no. Hooke18b/SCTM). Acknowledgements. C.A.G.-M., D.B.J. and S.D.T.G. are grateful to Invest NI and Randox Laboratories Ltd. for the award of a Research & Development Grant (059RDEN-1) that allowed the computational techniques employed to be developed. S.J. acknowledges support from the European Research Council under the European Union’s Horizon 2020 research and innovation programme (grant agreement no. 682462) and from the Research Council of Norway through its Centres of Excellence scheme (project no. 262622). J.M.R. and T.V.D. were supported by the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No 724326). T.V.D. received further support from the C1 grant TRACEspace of Internal Funds KU Leuven (number C14/19/089). The space-based data employed in this work is courtesy of NASA/SDO and the AIA, EVE and HMI science teams. 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 number 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 Hooke18b/SCTM). Publisher Copyright: © 2020 The Author(s). Copyright: Copyright 2021 Elsevier B.V., All rights reserved.

PY - 2021/2/8

Y1 - 2021/2/8

N2 - The suitability of solar pores as magnetic wave guides has been a key topic of discussion in recent years. Here, we present observational evidence of propagating magnetohydrodynamic wave activity in a group of five photospheric solar pores. Employing data obtained by the Facility Infrared Spectropolarimeter at the Dunn Solar Telescope, oscillations with periods of the order of 5 min were detected at varying atmospheric heights by examining Si 10827 Å line bisector velocities. Spectropolarimetric inversions, coupled with the spatially resolved root mean square bisector velocities, allowed the wave energy fluxes to be estimated as a function of atmospheric height for each pore. We find propagating magnetoacoustic sausage mode waves with energy fluxes on the order of 30kWm-2 at an atmospheric height of 100 km, dropping to approximately 2kWm-2 at an atmospheric height of around 500 km. The cross-sectional structuring of the energy fluxes reveals the presence of both body- A nd surface-mode sausage waves. Examination of the energy flux decay with atmospheric height provides an estimate of the damping length, found to have an average value across all five pores of L d ≈ 268km, similar to the photospheric density scale height. We find the damping lengths are longer for body mode waves, suggesting that surface mode sausage oscillations are able to more readily dissipate their embedded wave energies. This work verifies the suitability of solar pores to act as efficient conduits when guiding magnetoacoustic wave energy upwards into the outer solar atmosphere. This article is part of the Theo Murphy meeting issue 'High-resolution wave dynamics in the lower solar atmosphere'.

AB - The suitability of solar pores as magnetic wave guides has been a key topic of discussion in recent years. Here, we present observational evidence of propagating magnetohydrodynamic wave activity in a group of five photospheric solar pores. Employing data obtained by the Facility Infrared Spectropolarimeter at the Dunn Solar Telescope, oscillations with periods of the order of 5 min were detected at varying atmospheric heights by examining Si 10827 Å line bisector velocities. Spectropolarimetric inversions, coupled with the spatially resolved root mean square bisector velocities, allowed the wave energy fluxes to be estimated as a function of atmospheric height for each pore. We find propagating magnetoacoustic sausage mode waves with energy fluxes on the order of 30kWm-2 at an atmospheric height of 100 km, dropping to approximately 2kWm-2 at an atmospheric height of around 500 km. The cross-sectional structuring of the energy fluxes reveals the presence of both body- A nd surface-mode sausage waves. Examination of the energy flux decay with atmospheric height provides an estimate of the damping length, found to have an average value across all five pores of L d ≈ 268km, similar to the photospheric density scale height. We find the damping lengths are longer for body mode waves, suggesting that surface mode sausage oscillations are able to more readily dissipate their embedded wave energies. This work verifies the suitability of solar pores to act as efficient conduits when guiding magnetoacoustic wave energy upwards into the outer solar atmosphere. This article is part of the Theo Murphy meeting issue 'High-resolution wave dynamics in the lower solar atmosphere'.

KW - Sun: Atmosphere

KW - Sun: Magnetic fields

KW - Sun: Oscillations

KW - Sun: Photosphere

KW - sunspots

KW - techniques: Polarimetric

U2 - 10.1098/rsta.2020.0172

DO - 10.1098/rsta.2020.0172

M3 - Article

C2 - 33342383

AN - SCOPUS:85098744964

SN - 1364-503X

VL - 379

JO - Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences

JF - Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences

IS - 2190

M1 - 20200172

ER -

Magnetoacoustic wave energy dissipation in the atmosphere of solar pores

Abstract

Bibliographical note

Keywords

ASJC Scopus subject areas

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Magnetoacoustic Wave Energy Dissipation in the Atmosphere of Solar Pores

Student theses

Magnetoacoustic wave dynamics in the atmosphere of solar active regions

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