High-velocity blue-shifted Fe XXV He$\hat{I}\pm$ line during a superflare of the RS CVn-type star IM Peg

Abstract

Monitor of All-sky X-ray Image (MAXI) detected a superflare, releasing $5\times 10^{37}$ erg in 2$-$10 keV, of the RS CVn-type star IM Peg at 10:41 UT on 2023 July 23 with its Gas Slit Camera (GSC; 2$-$30 keV). We conducted X-ray follow-up observations of the superflare with Neutron Star Interior Composition ExploreR (NICER; 0.2$-$12 keV) starting at 16:52 UT on July 23 until 06:00 UT on August 2. NICER X-ray spectra clearly showed emission lines of the Fe XXV He$\hat{I}\pm$ and Fe XXVI Ly$\hat{I}\pm$ for $\sim 1.5$ days since the MAXI detection. The Fe XXV He$\hat{I}\pm$ line was blue-shifted with its maximum Doppler velocity reaching $-2200\pm 600$ $\mathrm{km}{\mathrm{s}}^{-1}$, 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$\hat{I}\pm$ line is blue-shifted during a stellar flare and its velocity overwhelmingly exceeds the escape velocity of the star ($-230$ $\mathrm{km}{\mathrm{s}}^{-1}$). 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.

14 pages, 9 figures. Accepted for publication in The Astrophysical Journal Letters