High-velocity Blue-shifted Fe xxv Heα Line during a Superflare of the RS Canum Venaticorum–type Star IM Peg
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Inoue, Shun, Wataru Buz Iwakiri, Teruaki Enoto, Hiroyuki Uchida, Miki Kurihara, Masahiro Tsujimoto, Yuta Notsu, et al. “High-Velocity Blue-Shifted Fe Xxv Heα Line during a Superflare of the RS Canum Venaticorum–Type Star IM Peg.” The Astrophysical Journal Letters 969, no. 1 (June 2024): L12. https://doi.org/10.3847/2041-8213/ad5667.
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CC BY 4.0 Deed ATTRIBUTION 4.0 INTERNATIONAL
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Abstract
The Monitor of All-sky X-ray Image (MAXI) detected a superflare, releasing 5 × 10³⁷ 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 (2−30 keV). We conducted X-ray follow-up observations of the superflare with the 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 Heα and Fe xxvi Lyα for ∼1.5 days since the MAXI detection. The Fe XXV Heα line was blueshifted with its maximum Doppler velocity reaching −2200 ± 600 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 Heα line is blueshifted during a stellar flare, and its velocity overwhelmingly exceeds the escape velocity of the star (−230 km s⁻¹). One hour before the most pronounced blueshift detection, a signature of the reheating of the flare plasma was observed. We discuss the origin of the blueshift, a CME, or high-velocity chromospheric evaporation.