Thermal and kinematic properties of ejecta in SN1987A revealed by XRISM
- Autori: Audard, M.; Awaki, H.; Ballhausen, R.; Bamba, A.; Behar, E.; Boissay-Malaquin, R.; Brenneman, L.; Brown, G.V.; Corrales, L.; Costantini, E.; Cumbee, R.; Diaz Trigo, M.; Done, C.; Dotani, T.; Ebisawa, K.; Eckart, M.E.; Eckert, D.; Enoto, T.; Eguchi, S.; Ezoe, Y.; Foster, A.; Fujimoto, R.; Fujita, Y.; Fukazawa, Y.; Fukushima, K.; Furuzawa, A.; Gallo, L.C.; Garcia, J.A.; Gu, L.; Guainazzi, M.; Giuffrida, R.; Hagino, K.; Hamaguchi, K.; Hatsukade, I.; Hayashi, K.; Hayashi, T.; Hell, N.; Hodges-Kluck, E.; Hornschemeier, A.; Ichinohe, Y.; Ishi, D.; Ishida, M.; Ishikawa, K.; Ishisaki, Y.; Kaastra, J.; Kallman, T.; Kara, E.; Katsuda, S.; Kanemaru, Y.; Kelley, R.; Kikuchi, R.; Kilbourne, C.; Kitamoto, S.; Kobayashi, S.; Kohmura, T.; Kubota, A.; Leutenegger, M.A.; Loewenstein, M.; Maeda, Y.; Markevitch, M.; Matsumoto, H.; Matsushima, T.; Matsushita, K.; Mccammon, D.; Mcnamara, B.; Mernier, F.; Miller, E.D.; Miller, J.M.; Mitsuishi, I.; Mizumoto, M.; Mizuno, T.; Mori, K.; Mukai, K.; Murakami, H.; Mushotzky, R.; Nakajima, H.; Nakazawa, K.; Ness, J.-.; Nobukawa, K.; Nobukawa, M.; Noda, H.; Odaka, H.; Ogawa, S.; Ogorzalek, A.; Okajima, T.; Ota, N.; Paltani, S.; Petre, R.; Plucinsky, P.; Porter, F.S.; Pottschmidt, K.; Sato, K.; Sato, T.; Sawada, M.; Seta, H.; Shidatsu, M.; Shimoda, J.; Simionescu, A.; Smith, R.K.; Suzuki, H.; Szymkowiak, A.; Takahashi, H.; Takeo, M.; Tamagawa, T.; Tamura, K.; Tanaka, T.; Tanimoto, A.; Tashiro, M.; Terada, Y.; Terashima, Y.; Tsuboi, Y.; Tsujimoto, M.; Tsunemi, H.; Tsuru, T.G.; Uchida, H.; Uchida, N.; Uchida, Y.; Uchiyama, H.; Ueda, S.; Ueda, Y.; Uno, S.; Vink, J.; Watanabe, S.; Williams, B.J.; Yamada, S.; Yamada, S.; Yamaguchi, H.; Yamaoka, K.; Yamasaki, N.; Yamauchi, M.; Yamauchi, S.; Yaqoob, T.; Yoneyama, T.; Yoshida, T.; Yukita, M.; Zhuravleva, I.; Miceli, M.; Sapienza, V.
- Anno di pubblicazione: 2025
- Tipologia: Articolo in rivista
- OA Link: http://hdl.handle.net/10447/700267
Abstract
We present an analysis of high-resolution spectra from the shock-heated plasmas in SN 1987A, based on an observation using the Resolve instrument onboard the X-Ray Imaging and Spectroscopy Mission (XRISM). The 1.7-10 keV Resolve spectra are accurately represented by a single-component, plane-parallel shock plasma model, with a temperature of keV and an ionization parameter of ×. The Resolve spectra are also well reproduced by the 3D magneto-hydrodynamic simulation presented by Orlando et al. (2020, A&A, 636, A22) suggesting substantial contribution from the ejecta. The metal abundances obtained with Resolve align with the Large Magellanic Cloud value, indicating that the X-rays in 2024 originate from "non-metal-rich"shock-heated ejecta and the reverse shock has not reached the inner metal-rich region of ejecta. Doppler widths of the atomic lines from Si, S, and Fe correspond to velocities of 1500-1700 km s, where the thermal broadening effects in this non-metal-rich plasma are negligible. Therefore, the line broadening seen in Resolve spectra is determined by the large bulk motion of ejecta. For reference, we determined a upper limit on non-thermal emission from a pulsar wind nebula at erg cm s in the 2-10 keV range, aligning with NuSTAR findings by Greco et al. (2022, ApJ, 931, 132). Additionally, we searched for the Sc K line feature and found a upper limit of photons cm s, which translates to an initial Ti mass of approximately, consistent with previous X-ray to soft gamma-ray observations (Boggs et al. 2015, Science, 348, 670; Grebenev et al. 2012, Nature, 490, 373; Leising 2006, ApJ, 651, 1019).