Transient Mass Loss Analysis of Solar Observations using Stellar Methods

TL;DR

This study evaluates a multi-wavelength method for analyzing stellar coronal mass ejections using solar observations, confirming its accuracy for speed and providing insights into mass and energy estimates, aiding stellar event interpretation.

Contribution

It validates and assesses the accuracy of a proposed stellar CME analysis methodology using solar data, highlighting its reliability for speed and limitations for mass and energy estimates.

Findings

CME speed estimates are accurate within a few hundred km/s.

Mass and kinetic energy estimates are only approximate due to large errors.

Method is applicable for interpreting stellar CME observations.

Abstract

Low frequency dynamic spectra of radio bursts from nearby stars offer the best chance to directly detect the stellar signature of transient mass loss on low mass stars. Crosley et al. (2016) proposes a multi-wavelength methodology to determine coronal mass ejection parameters, such as Coronal Mass Ejection (CME) speed, mass, and kinetic energy. We test the validity and accuracy of the results derived from the methodology by using Geostationary Operational Environmental Satellite X-ray observations and Bruny Island Radio Spectrometer radio observations. These are analogous observations to those which would be found in the stellar studies. Derived results from these observations are compared to direct white light measurements of the Large Angle and Spectrometric Coronagraph. We find that, when a pre-event temperature can be determined, that the accuracy of CME speeds are within a few hundred km/s, and are reliable when specific criteria has been met. CME mass and kinetic energies are only useful in determining approximate order of magnitude measurements when considering the large errors associated to them. These results will be directly applicable to interpretation of any detected stellar events and derivation of stellar CME properties.