Chromospheric resonator model for sunspot revealed by multi-height observation of umbral wave

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ID: 314415
2026
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Abstract
Abstract Sunspots are transient, magnetically intense features that host oscillations linked to magnetohydrodynamic (MHD) waves. These waves may contribute to plasma heating and drive mass flows in the solar wind. Beyond their energetic role, they serve as diagnostic tools for probing sunspot structure. In this study, we investigated chromospheric wave propagation in a sunspot using high-resolution, multi-wavelength observations from the Goode Solar Telescope at Big Bear Solar Observatory. Spectral analysis shows that the intensity at Hα line core and its wings exhibited oscillatory signal at about 3 min. We performed a cross-wavelet analysis to examine the phase relationship between the wing-integrated and line-core intensity oscillations of the Hα line and the centroid-derived Hα Doppler velocity. We also analyze the phase relationships between intensity pairs from different passband combinations of the Hα line. The results indicate the presence of slow magnetoacoustic modes manifesting standing waves along with upward propagating waves. The observed phase patterns suggest that umbral waves are confined within a non-ideal acoustic resonator, providing measurable wave properties that could serve as input for sunspot seismology and refine models of sunspot atmospheric structure.
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Authors Kartika Sangal, A K Srivastava, Libo Fu, Ding Yuan, Song Feng, Yuandeng Shen
Journal monthly notices of the royal astronomical society
Year 2026
DOI
10.1093/mnras/stag962
URL
https://doi.org/10.1093/mnras/stag962
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