A study of X-ray flares - I. Active late-type dwarfs

TL;DR

This study analyzes X-ray flares from six active late-type dwarf stars, revealing frequent flaring activity, spectral evolution, and loop sizes smaller than the stars, with evidence of sustained heating during decay phases.

Contribution

It provides detailed temporal and spectral analysis of flares from late-type dwarfs, including loop size estimation and evidence of sustained heating, expanding understanding of stellar flare mechanisms.

Findings

Frequent flaring observed in all six stars.

Largest flare had a decay time of 10 ks and doubled the quiescent luminosity.

Flares involve loops smaller than the stellar radius with sustained heating.

Abstract

We present temporal and spectral characteristics of X-ray flares observed from six late-type G-K active dwarfs (V368 Cep, XI Boo, IM Vir, V471 Tau, CC Eri and EP Eri) using data from observations with the XMM-Newton observatory. All the stars were found to be flaring frequently and altogether a total of seventeen flares were detected above the ``quiescent'' state X-ray emission which varied from 0.5 to 8.3 x 10^{29} erg/s. The largest flare was observed in a low activity dwarf XI Boo with a decay time of 10 ks and ratio of peak flare luminosity to ``quiescent'' state luminosity of 2. We have studied the spectral changes during the flares by using colour-colour diagram and by detailed spectral analysis during the temporal evolution of the flares. The exponential decay of the X-ray light curves, and time evolution of the plasma temperature and emission measure are similar to those observed in compact solar flares. We have derived the semiloop lengths of flares based on the hydrodynamic flare model. The size of the flaring loops is found to be less than the stellar radius. The hydrodynamic flare decay analysis indicates the presence of sustained heating during the decay of most flares.