Journal
ASTROPHYSICAL JOURNAL
Volume 847, Issue 1, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.3847/1538-4357/aa86b5
Keywords
magnetohydrodynamics (MHD); methods: observational; Sun: atmosphere; Sun: oscillations sunspots
Categories
Funding
- UK Science and Technology Facilities Council (STFC)
- UK STFC
- Invest NI [059RDEN-1]
- Randox Laboratories Ltd. [059RDEN-1]
- Odysseus grant of the FWO Vlaanderen
- Belspo [IAP P7/08 CHARM]
- KU Leuven [GOA-2015-014]
- European Research Council (ERC) under the European Union's Horizon research and innovation programme [724326]
- Leverhulme Trust Early Career Fellowship
- STFC
- Royal Society-Newton Mobility Grant [NI160149]
- STFC (UK)
- Royal Society (UK)
- ESA
- Norwegian Space Centre
- Science and Technology Facilities Council [ST/J001430/1, ST/M000826/1] Funding Source: researchfish
- STFC [ST/J001430/1, ST/M000826/1, ST/K004220/1, ST/P000304/1] Funding Source: UKRI
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High spatial and temporal resolution images of a sunspot, obtained simultaneously in multiple optical and UV wavelengths, are employed to study the propagation and damping characteristics of slow magnetoacoustic waves up to transition region heights. Power spectra are generated from intensity oscillations in sunspot umbra, across multiple atmospheric heights, for frequencies up to a few hundred mHz. It is observed that the power spectra display a power-law dependence over the entire frequency range, with a significant enhancement around 5.5 mHz found for the chromospheric channels. The phase difference spectra reveal a cutoff frequency near 3 mHz, up to which the oscillations are evanescent, while those with higher frequencies propagate upward. The power-law index appears to increase with atmospheric height. Also, shorter damping lengths are observed for oscillations with higher frequencies suggesting frequency-dependent damping. Using the relative amplitudes of the 5.5 mHz (3 minute) oscillations, we estimate the energy flux at different heights, which seems to decay gradually from the photosphere, in agreement with recent numerical simulations. Furthermore, a comparison of power spectra across the umbral radius highlights an enhancement of high-frequency waves near the umbral center, which does not seem to be related to magnetic field inclination angle effects.
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