Magnetic and Kinetic Power Spectra as a Tool to Probe the Turbulent Dynamo

TL;DR

This paper investigates the potential presence of a small-scale turbulent dynamo in the quiet Sun by analyzing magnetic and velocity energy spectra from various high-resolution solar observations.

Contribution

It introduces a spectral analysis approach to probe the turbulent dynamo in the quiet Sun using multiple observational datasets.

Findings

Magnetic and velocity spectra show signatures consistent with turbulent dynamo activity.

Analysis suggests the turbulent dynamo could operate in the quiet Sun.

Results provide observational constraints for solar dynamo models.

Abstract

Generation and diffusion of the magnetic field on the Sun is a key mechanism responsible for solar activity on all spatial and temporal scales - from the solar cycle down to the evolution of small-scale magnetic elements in the quiet Sun. The solar dynamo operates as a non-linear dynamical process and is thought to be manifest in two types: as a global dynamo responsible for the solar cycle periodicity, and as a small-scale turbulent dynamo responsible for the formation of magnetic carpet in the quiet Sun. Numerous MHD simulations of the solar turbulence did not yet reach a consensus as to the existence of a turbulent dynamo on the Sun. At the same time, high-resolution observations of the quiet Sun from Hinode instruments suggest possibilities for the turbulent dynamo. Analysis of characteristics of turbulence derived from observations would be beneficial in tackling the problem. We analyse magnetic and velocity energy spectra as derived from Hinode/SOT, SOHO/MDI, SDO/HMI and the New Solar Telescope (NST) of Big Bear Solar Observatory (BBSO) to explore the possibilities for the small-scale turbulent dynamo in the quiet Sun.