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Problems in Observation and Identification of Torsional Waves in the Lower Solar Atmosphere View all abstracts by submitter

Andrei Chelpanov   Submitted: 2022-12-28 23:13

Registering periodic variations of spectral line widths serves as the main method for observing torsional Alfvén waves. Theoretically, the method seems valid, yet it entails a number of caveats when applied to data. For instance, the amplitudes of these observations should vary with changes of the location on the disk, and they should be associated with no intensity oscillations. We analyze extensive observational material of periodic non-thermal variations of line widths in coronal holes and facular regions in a number of spectral lines: Hα, He I 10830 , Ca II 8542 , Ba II 4554 . In most cases, we detected associated intensity oscillations at similar frequencies. Besides, we observed no centre-to-limb dependency. This calls for a discussion on the practical validity of the method and on the alternative explanations for the nature of non-thermal variations of spectral line widths. Based on our observations, we consider registering line profile broadening a necessary but not sufficient means for unambiguous identification of torsional Alfvén waves in the lower solar atmosphere.

Authors: A.A. Chelpanov, N.I. Kobanov
Projects: None

Publication Status: Published in Solar Physics
Last Modified: 2023-01-02 23:05
Go to main E-Print page  Unfolding Drift Effects for Cosmic Rays over the Period of the Sun's Magnetic Field Reversal  Solar Orbiter and SDO Observations, and Bifrost MHD Simulations of Small-scale Coronal Jets  Edit Entry  Download Preprint  Delete Entry 

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