Saturation Levels for White-light Flares of Flare Stars: Variation of Minimum Flare Duration for Saturation

TL;DR

This study investigates the saturation levels of white-light flares in UV Ceti stars, revealing a maximum energy limit and how minimum flare durations for saturation vary with spectral type, based on two years of observational data.

Contribution

It introduces the concept of a saturation energy level for white-light flares and analyzes how minimum flare durations for saturation change across different spectral types.

Findings

Flare energies are capped at a saturation level regardless of flare duration.

The span of equivalent durations is similar across different stars.

Minimum flare durations for saturation increase with later spectral types.

Abstract

Taking into account results obtained from models and from statistical analyses of obtained parameters, we discuss flare activity levels and flare characteristics of five UV Ceti stars. We present the parameters of unpublished flares detected over two years of observations of V1005 Ori. We compare parameters of the U-band flares detected over several seasons of observations of AD Leo, EV Lac, EQ Peg, V1054 Oph, and V1005 Ori. Flare frequencies calculated for all program stars and maximum energy levels of the flares are compared, and we consider which is the most correct parameter as an indicator of flare activity levels. Using the One Phase Exponential Association function, the distributions of flare equivalent duration versus flare total duration are modeled for each program star. We use the Independent Samples t-Test in the statistical analyses of the parameters obtained from the models. The results reveal some properties of flare processes occurring on the surfaces of UV Ceti type stars. (1) Flare energies cannot be higher than a specific value regardless of the length of the flare total duration. This must be a saturation level for white-light flares occurring in flare processes observed in the U band. Thus, for the first time it is shown that white-light flares have a saturation in a specific energy range. (2) The span values, which are the difference between the equivalent durations of flares with the shortest and longest total durations, are almost equal for each star. (3) The half-life values, minimum flare durations for saturation, increase toward the later spectral types.