Please use this identifier to cite or link to this item:
http://hdl.handle.net/2248/8093
Full metadata record
DC Field | Value | Language |
---|---|---|
dc.contributor.author | Grant, S. D. T | - |
dc.contributor.author | Jess, D. B | - |
dc.contributor.author | Stangalini, M | - |
dc.contributor.author | Jafarzadeh, S | - |
dc.contributor.author | Fedun, V | - |
dc.contributor.author | Verth, G | - |
dc.contributor.author | Keys, P. H | - |
dc.contributor.author | Rajaguru, S. P | - |
dc.contributor.author | Uitenbroek, H | - |
dc.contributor.author | MacBride, C. D | - |
dc.contributor.author | Bate, W | - |
dc.contributor.author | Gilchrist-Millar, C. A | - |
dc.date.accessioned | 2022-12-01T05:34:08Z | - |
dc.date.available | 2022-12-01T05:34:08Z | - |
dc.date.issued | 2022-10-20 | - |
dc.identifier.citation | The Astrophysical Journal, Vol. 938, No. 2, 143 | en_US |
dc.identifier.issn | 1538-4357 | - |
dc.identifier.uri | http://hdl.handle.net/2248/8093 | - |
dc.description | Open Access | en_US |
dc.description | Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. | - |
dc.description.abstract | Solar pores are efficient magnetic conduits for propagating magnetohydrodynamic wave energy into the outer regions of the solar atmosphere. Pore observations often contain isolated and/or unconnected structures, preventing the statistical examination of wave activity as a function of the atmospheric height. Here, using high-resolution observations acquired by the Dunn Solar Telescope, we examine photospheric and chromospheric wave signatures from a unique collection of magnetic pores originating from the same decaying sunspot. Wavelet analysis of high-cadence photospheric imaging reveals the ubiquitous presence of slow sausage-mode oscillations, coherent across all photospheric pores through comparisons of intensity and area fluctuations, producing statistically significant in-phase relationships. The universal nature of these waves allowed an investigation of whether the wave activity remained coherent as they propagate. Utilizing bisector Doppler velocity analysis of the Ca ii 8542 Å line, alongside comparisons of the modeled spectral response function, we find fine-scale 5 mHz power amplification as the waves propagate into the chromosphere. Phase angles approaching zero degrees between co-spatial line depths spanning different line depths indicate standing sausage modes following reflection against the transition region boundary. Fourier analysis of chromospheric velocities between neighboring pores reveals the annihilation of the wave coherency observed in the photosphere, with examination of the intensity and velocity signals from individual pores indicating they behave as fractured waveguides, rather than monolithic structures. Importantly, this work highlights that wave morphology with atmospheric height is highly complex, with vast differences observed at chromospheric layers, despite equivalent wave modes being introduced into similar pores in the photosphere. | en_US |
dc.language.iso | en | en_US |
dc.publisher | American Astronomical Society | en_US |
dc.relation.uri | https://doi.org/10.3847/1538-4357/ac91ca | - |
dc.rights | © 2022. The Author(s) | - |
dc.subject | Solar chromosphere | en_US |
dc.subject | Magnetohydrodynamics | en_US |
dc.subject | Solar oscillations | en_US |
dc.subject | Solar photosphere | en_US |
dc.subject | Solar magnetic fields | en_US |
dc.title | The Propagation of Coherent Waves Across Multiple Solar Magnetic Pores | en_US |
dc.type | Article | en_US |
Appears in Collections: | IIAP Publications |
Files in This Item:
File | Description | Size | Format | |
---|---|---|---|---|
The Propagation of Coherent Waves Across Multiple Solar Magnetic Pores.pdf | 3.01 MB | Adobe PDF | View/Open |
Items in DSpace are protected by copyright, with all rights reserved, unless otherwise indicated.