High-velocity blue-shifted Fe XXV He$\alpha$ line during a superflare of the RS CVn-type star IM Peg

TL;DR

This study reports the first detection of a highly blue-shifted Fe XXV Heα line during a stellar superflare, indicating plasma velocities exceeding the star's escape velocity, likely due to a CME or chromospheric evaporation.

Contribution

It presents the first observation of a blue-shifted Fe XXV Heα line during a stellar flare, revealing plasma velocities surpassing the star's escape velocity.

Findings

Fe XXV Heα line was blue-shifted with velocities up to -2200 km/s.

The blue-shifted line indicates upward-moving plasma, possibly a CME.

Velocity exceeds the star's escape velocity, implying plasma escape.

Abstract

Monitor of All-sky X-ray Image (MAXI) detected a superflare, releasing $5\times 10^{37}$ erg in 2$-$10 keV, of the RS CVn-type star IM Peg at 10:41 UT on 2023 July 23 with its Gas Slit Camera (GSC; 2$-$30 keV). We conducted X-ray follow-up observations of the superflare with Neutron Star Interior Composition ExploreR (NICER; 0.2$-$12 keV) starting at 16:52 UT on July 23 until 06:00 UT on August 2. NICER X-ray spectra clearly showed emission lines of the Fe XXV He$\alpha$ and Fe XXVI Ly$\alpha$ for $\sim 1.5$ days since the MAXI detection. The Fe XXV He$\alpha$ line was blue-shifted with its maximum Doppler velocity reaching $-2200 \pm 600$ $\mathrm{km \: s^{-1}}$, suggesting an upward-moving plasma during the flare, such as a coronal mass ejection (CME) and/or chromospheric evaporation. This is the first case that the Fe XXV He$\alpha$ line is blue-shifted during a stellar flare and its velocity overwhelmingly exceeds the escape velocity of the star ($-230$ $\mathrm{km \: s^{-1}}$). One hour before the most pronounced blueshift detection, a signature of reheating the flare plasma was observed. We discuss the origin of the blueshift, a CME or high-velocity chromospheric evaporation.