Journal
ASTROPHYSICAL JOURNAL LETTERS
Volume 724, Issue 2, Pages L194-L198Publisher
IOP PUBLISHING LTD
DOI: 10.1088/2041-8205/724/2/L194
Keywords
line: formation; magnetohydrodynamics (MHD); Sun: corona; Sun: oscillations
Categories
Funding
- UK Engineering and Physical Sciences Research Council (EPSRC)
- UK Science and Technology Facilities Council (STFC) [ST/F002769/1]
- STFC on the CFSA
- European Community [220555]
- Royal Society University
- Engineering and Physical Sciences Research Council [EP/D062837/1] Funding Source: researchfish
- Science and Technology Facilities Council [ST/F00205X/1, PP/E001122/1, ST/H001964/1, ST/F002769/1] Funding Source: researchfish
- EPSRC [EP/D062837/1] Funding Source: UKRI
- STFC [ST/F00205X/1, PP/E001122/1, ST/H001964/1, ST/F002769/1] Funding Source: UKRI
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Recent spectral observations of upward moving quasi-periodic intensity perturbations in solar coronal structures have shown evidence of periodic line asymmetries near their footpoints. These observations challenge the established interpretation of the intensity perturbations in terms of propagating slow magnetoacoustic waves. We show that slow waves inherently have a bias toward enhancement of emission in the blue wing of the emission line due to in-phase behavior of velocity and density perturbations. We demonstrate that slow waves cause line asymmetries when the emission line is averaged over an oscillation period or when a quasi-static plasma component in the line of sight is included. Therefore, we conclude that slow magnetoacoustic waves remain a valid explanation for the observed quasi-periodic intensity perturbations.
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