The Thermal Properties of Solar Flares Over Three Solar Cycles Using GOES X-ray Observations

TL;DR

This study introduces an automated method (TEBBS) for analyzing GOES X-ray data to derive thermal properties of over 50,000 solar flares across three solar cycles, revealing new scaling relationships and trends.

Contribution

The paper presents a novel automated background subtraction method (TEBBS) for GOES X-ray data, enabling large-scale analysis of solar flare thermal properties over three solar cycles.

Findings

Peak emission measure and radiative losses scale with GOES flux as power-laws.

Peak temperature scales logarithmically with GOES flux.

Flares of a given GOES class have lower peak temperatures and higher emission measures than previously reported.

Abstract

Solar flare X-ray emission results from rapidly increasing temperatures and emission measures in flaring active region loops. To date, observations from the X-Ray Sensor (XRS) onboard the Geostationary Operational Environmental Satellite (GOES) have been used to derive these properties, but have been limited by a number of factors, including the lack of a consistent background subtraction method capable of being automatically applied to large numbers of flares. In this paper, we describe an automated temperature and emission measure-based background subtraction method (TEBBS), which builds on the methods of Bornmann (1990). Our algorithm ensures that the derived temperature is always greater than the instrumental limit and the pre-flare background temperature, and that the temperature and emission measure are increasing during the flare rise phase. Additionally, TEBBS utilizes the improved estimates of GOES temperatures and emission measures from White et al. (2005). TEBBS was successfully applied to over 50,000 solar flares occurring over nearly three solar cycles (1980-2007), and used to create an extensive catalog of the solar flare thermal properties. We confirm that the peak emission measure and total radiative losses scale with background subtracted GOES X-ray flux as power-laws, while the peak temperature scales logarithmically. As expected, the peak emission measure shows an increasing trend with peak temperature, although the total radiative losses do not. While these results are comparable to previous studies, we find that flares of a given GOES class have lower peak temperatures and higher peak emission measures than previously reported. The resulting TEBBS database of thermal flare plasma properties is publicly available on Solar Monitor (www.solarmonitor.org/TEBBS/) and will be available on Heliophysics Integrated Observatory (www.helio-vo.eu).