Delayed Development of Cool Plasmas in X-ray Flares from kappa1 Ceti

TL;DR

This study analyzes two powerful X-ray flares from kappa1 Ceti, revealing delayed cool plasma development and providing insights into flare loop geometry and cooling mechanisms through spectral and hydrodynamic modeling.

Contribution

It presents detailed spectral analysis of stellar superflares and links plasma cooling delays to magnetic loop structures, advancing understanding of stellar flare physics.

Findings

Cool plasma lags by ~200 sec behind hot plasma.

Cool component has smaller emission measure, indicating suppressed conduction.

Time lag constrains flare loop geometry.

Abstract

The Neutron star Interior Composition ExploreR (NICER) X-ray observatory observed two powerful X-ray flares equivalent to superflares from the nearby young solar-like star, kappa1 Ceti, in 2019. NICER follows each flare from the onset through the early decay, collecting over 30 cts s-1 near the peak, enabling a detailed spectral variation study of the flare rise. The flare in September varies quickly in ~800 sec, while the flare in December has a few times longer timescale. In both flares, the hard band (2-4 keV) light curves show typical stellar X-ray flare variations with a rapid rise and slow decay, while the soft X-ray light curves, especially of the September flare, have prolonged flat peaks. The time-resolved spectra require two temperature plasma components at kT ~0.3-1 keV and ~2-4 keV. Both components vary similarly, but the cool component lags by ~200 sec with a 4-6 times smaller emission measure (EM) compared to the hot component. A comparison with hydrodynamic flare loop simulations indicates that the cool component originates from X-ray plasma near the magnetic loop footpoints, which mainly cools via thermal conduction. The time lag represents the travel time of the evaporated gas through the entire flare loop. The cool component has several times smaller EM than its simulated counterpart, suggesting a suppression of conductive cooling possibly by the expansion of the loop cross-sectional area or turbulent fluctuations. The cool component's time lag and small EM ratio provide important constraints on the flare loop geometry.