XRISM view of a stellar flare: High-resolution Fe K spectra of HR 1099, an RS CVn-type star
Fuente:
arXiv
Guardado en:
| Autores principales: | , , , , , , , , , , , , , , , , , , , , , , , |
|---|---|
| Formato: | Preprint |
| Publicado: |
2025
|
| Materias: | |
| Acceso en línea: | |
| Etiquetas: |
Agregar Etiqueta
Sin Etiquetas, Sea el primero en etiquetar este registro!
|
| _version_ | 1866908718027767808 |
|---|---|
| author | Kurihara, Miki Tsujimoto, Masahiro Loewenstein, Michael Maeda, Yoshitomo Audard, Marc Behar, Ehud Eckart, Megan E. Foster, Adam Gu, Liyi Guainazzi, Matteo Hamaguchi, Kenji Hell, Natalie Inoue, Shun Ishihara, Yukiko Katsuda, Satoru Kilbourne, Caroline A. Leutenegger, Maurice A. Miller, Eric D. Nagashima, Nagisa Porter, Frederick Scott Sawada, Makoto Tsuboi, Yohko Kashyap, Vinay L. Brooks, David H. |
| author_facet | Kurihara, Miki Tsujimoto, Masahiro Loewenstein, Michael Maeda, Yoshitomo Audard, Marc Behar, Ehud Eckart, Megan E. Foster, Adam Gu, Liyi Guainazzi, Matteo Hamaguchi, Kenji Hell, Natalie Inoue, Shun Ishihara, Yukiko Katsuda, Satoru Kilbourne, Caroline A. Leutenegger, Maurice A. Miller, Eric D. Nagashima, Nagisa Porter, Frederick Scott Sawada, Makoto Tsuboi, Yohko Kashyap, Vinay L. Brooks, David H. |
| contents | 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 $\sim$400 ks telescope time covering 1.5 binary orbit, a flare lasting for $\sim$100 ks was observed with a released X-ray radiation energy of $\sim 10^{34}$ 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. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2512_15204 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | XRISM view of a stellar flare: High-resolution Fe K spectra of HR 1099, an RS CVn-type star Kurihara, Miki Tsujimoto, Masahiro Loewenstein, Michael Maeda, Yoshitomo Audard, Marc Behar, Ehud Eckart, Megan E. Foster, Adam Gu, Liyi Guainazzi, Matteo Hamaguchi, Kenji Hell, Natalie Inoue, Shun Ishihara, Yukiko Katsuda, Satoru Kilbourne, Caroline A. Leutenegger, Maurice A. Miller, Eric D. Nagashima, Nagisa Porter, Frederick Scott Sawada, Makoto Tsuboi, Yohko Kashyap, Vinay L. Brooks, David H. Solar and Stellar Astrophysics High Energy Astrophysical Phenomena 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 $\sim$400 ks telescope time covering 1.5 binary orbit, a flare lasting for $\sim$100 ks was observed with a released X-ray radiation energy of $\sim 10^{34}$ 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. |
| title | XRISM view of a stellar flare: High-resolution Fe K spectra of HR 1099, an RS CVn-type star |
| topic | Solar and Stellar Astrophysics High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2512.15204 |