Propagating kink waves in the solar corona

Tiwari, Ajay Kumar (2020) Propagating kink waves in the solar corona. Doctoral thesis, Northumbria University.

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Abstract

The solar atmosphere is known to host various modes of MHD waves. Transverse waves are thought to play an important role in energy transfer in the atmosphere and thus in solar coronal heating and the acceleration of the solar wind. The transverse waves studied so far have predominantly been interpreted as standing kink waves and, via coronal magneto-seismology, they can offer insight into the physical conditions of coronal plasmas. In addition, the excitation of these standing kink waves are associated with low coronal eruptions and thus need special conditions or drivers.
Propagating kink waves have been reported recently and have been found to be ubiquitous in the solar corona including in the quiet Sun. It is imperative to understand the mechanisms that enable their energy to be transferred to the plasma. Carrying on the legacy of the standing kink waves, mode conversion via resonant absorption is thought to be one of the main mechanisms for damping of these propagating kink waves, and is considered to play a key role in the process of energy transfer. The propagating kink waves are best observed in the Doppler velocity images of the Coronal Multi-channel Polarimeter (CoMP). The damping is observed using data from this instrument to study the energetics of the propagating kink waves in quiescent coronal loops.
A coherence-based method is used to track the Doppler velocity signal of the waves, enabling an investigation into the spatial evolution of velocity perturbations. To enable accurate estimates of these quantities, the first derivation is provided of a likelihood function suitable for fitting models to the ratio of two power spectra obtained from discrete Fourier transforms. Maximum likelihood estimation is used to fit an exponential damping model to the observed variation in power ratio as a function of frequency. This also confirms earlier indications that propagating kink waves are undergoing frequency-dependent damping. Additionally, it is found that the rate of damping decreases, or equivalently the damping length increases, for longer coronal loops that reach higher in the corona.
The analysis techniques are used to create a statistical sample of quiescent loops to study the statistical properties of propagating kink waves and compare it to the studies of standing kink waves. It is noted that the damping for the propagating waves appears to be significantly weaker than that found from measurements of
standing kink modes. The propagating kink waves also exhibit signatures of power amplification of waves.

Item Type: Thesis (Doctoral)
Uncontrolled Keywords: solar physics, solar corona, mhd waves, solar atmosphere, quiet sun
Subjects: F300 Physics
F500 Astronomy
Department: Faculties > Engineering and Environment > Mathematics, Physics and Electrical Engineering
University Services > Graduate School > Doctor of Philosophy
Depositing User: John Coen
Date Deposited: 04 Jan 2021 11:08
Last Modified: 04 Jan 2021 11:15
URI: http://nrl.northumbria.ac.uk/id/eprint/45071

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