Large-amplitude transverse MHD waves prevailing in the Hα chromosphere of a solar quiet region revealed by MiHI integrated field spectral observations

¹ Astronomy Program, Department of Physics and Astronomy, Seoul National University, Gwanak-gu, Seoul 08826, Korea
e-mail: jcchae@snu.ac.kr
² Max-Planck Institute for Solar System Research, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany
³ Space Research and Technology Institute, Bulgarian Academy of Sciences, Acad. Georgy Bonchev Str., Bl. 1, 1113 Sofia, Bulgaria
⁴ Bay Area Environmental Research Institute, NASA Research Park, Moffett Field, CA 94035, USA
⁵ Lockheed Martin Solar & Astrophysics Laboratory, 3251 Hanover Street Palo Alto, CA 94304, USA

Received: 28 February 2024
Accepted: 6 May 2024

Abstract

The investigation of plasma motions in the solar chromosphere is crucial for understanding the transport of mechanical energy from the interior of the Sun to the outer atmosphere and into interplanetary space. We report the finding of large-amplitude oscillatory transverse motions prevailing in the non-spicular Hα chromosphere of a small quiet region near the solar disk center. The observation was carried out on 2018 August 25 with the Microlensed Hyperspectral Imager (MiHI) installed as an extension to the spectrograph at the Swedish Solar Telescope (SST). MiHI produced high-resolution Stokes spectra of the Hα line over a two-dimensional array of points (sampled every 0.066″ on the image plane) every 1.33 s for about 17 min. We extracted the Doppler-shift-insensitive intensity data of the line core by applying a bisector fit to Stoke I line profiles. From our time–distance analysis of the intensity data, we find a variety of transverse motions with velocity amplitudes of up to 40 km s⁻¹ in fan fibrils and tiny filaments. In particular, in the fan fibrils, large-amplitude transverse MHD waves were seen to occur with a mean velocity amplitude of 25 km s⁻¹ and a mean period of 5.8 min, propagating at a speed of 40 km s⁻¹. These waves are nonlinear and display group behavior. We estimate the wave energy flux in the upper chromosphere at 3 × 10⁶ erg cm⁻² s⁻¹. Our results contribute to the advancement of our understanding of the properties of transverse MHD waves in the solar chromosphere.