XRISM view of a stellar flare: High-resolution Fe K spectra of HR 1099, an RS CVn-type star

Files

psaf124.pdf (2.64 MB)

Links to Files

https://academic.oup.com/pasj/advance-article/doi/10.1093/pasj/psaf124/8342007

Permanent Link

https://doi.org/10.1093/pasj/psaf124
 http://hdl.handle.net/11603/41422

Collections

UMBC Faculty Collection
UMBC Center for Space Sciences and Technology (CSST) / Center for Research and Exploration in Space Sciences & Technology II (CRSST II)
UMBC Physics Department

Author/Creator

Author/Creator ORCID

https://orcid.org/0000-0001-7515-2779

Date

2025-11-25

Type of Work

journal articles
Text

Department

Program

Citation of Original Publication

Kurihara, Miki, Masahiro Tsujimoto, Michael Loewenstein, et al. “XRISM View of a Stellar Flare: High-Resolution Fe K Spectra of HR 1099, an RS CVn-Type Star.” Publications of the Astronomical Society of Japan, November 25, 2025, psaf124. https://doi.org/10.1093/pasj/psaf124.

Rights

This work was written as part of one of the author's official duties as an Employee of the United States Government and is therefore a work of the United States Government. In accordance with 17 U.S.C. 105, no copyright protection is available for such works under U.S. Law.
Public Domain

Subjects

Abstract

A high-resolution X-ray spectroscopic observation was made of the RS CVn-type binary star HR 1099 using the Resolve instrument onboard XRISM for its calibration purposes. During the ~400 ks telescope time covering 1.5 binary orbit, a flare lasting for ~100 ks was observed with a released X-ray radiation energy of ~10³⁴ erg, making it the first stellar flare ever observed with an X-ray microcalorimeter spectrometer. The flare peak count rate is 6.4 times higher than that in quiescence and is distinguished clearly in time thanks to the long telescope time. Many emission lines were detected in the 1.7–10 keV range both in the flare and quiescent phases. Using the high spectral resolution of Resolve in the Fe K band (6.5–7.0 keV), we resolved the inner-shell lines of Fe?xix–xxiv as well as the outer-shell lines of Fe?xxv–xxvi. These lines have peaks in the contribution functions at different temperatures over a wide range, allowing us to construct the differential emission measure (DEM) distribution over the electron temperature of 1–10 keV (roughly 10–100 MK) based only on Fe lines, thus without an assumption of the elemental abundance. The reconstructed DEM has a bimodal distribution, and only the hotter component increased during the flare. The elemental abundance was derived based on the DEM distribution thus constructed. A significant abundance increase was observed during the flare for Ca and Fe, which are some of the elements with the lowest first ionization potential among those analyzed, but not for Si, S, and Ar. This behavior is seen in some giant solar flares and the present result is a clear example in stellar flares.