Determination of Prominence Plasma Beta from the Dynamics of Rising Plumes

TL;DR

This paper introduces a method to estimate the plasma beta in solar prominences by analyzing the dynamics of rising plumes, combining fluid dynamics with MHD corrections, validated through simulations and applied to observational data.

Contribution

The paper presents a novel approach to determine prominence plasma beta from observed plume dynamics using a fluid dynamic model with MHD corrections, validated by simulations.

Findings

Estimated plasma beta range: 0.47 to 1.13

Method validated through simulations

Potential to improve understanding of prominence MHD phenomena

Abstract

The launch of Hinode satellite led to the discovery of rising plumes, dark in chromospheric lines, in quiescent prominences that propagate from large (~10 Mm) bubbles that form at the base of the prominences. These plumes present a very interesting opportunity to study Magnetohydrodynamic (MHD) phenomena in quiescent prominences, but obstacles still remain. One of the biggest issues is that of the magnetic field strength, which is not easily measurable in prominences. In this paper we present a method that may be used to determine a prominence's plasma \beta when rising plumes are observed. Using the classic fluid dynamic solution for flow around a circular cylinder with an MHD correction, the compression of the prominence material can be estimated. This has been successfully confirmed through simulations; application to a prominence gave an estimate of the plasma beta as \beta=0.47 to 1.13 with an error of 0.080 for the range \gamma=1.4 to 1.7. Using this method it may be possible to estimate the plasma beta of observed prominences, therefore helping our understanding of a prominence's dynamics in terms of MHD phenomena.