Thermonuclear superburst of MAXI J1752$-$457 observed with NinjaSat and MAXI
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| Format: | Preprint |
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2025
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| _version_ | 1866909691045478400 |
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| author | Aoyama, Amira Enoto, Teruaki Takahashi, Takuya Watanabe, Sota Takeda, Tomoshi Iwakiri, Wataru Yamasaki, Kaede Iwata, Satoko Ota, Naoyuki Jujo, Arata Tamagawa, Toru Mihara, Tatehiro Hu, Chin-Ping Dohi, Akira Nishimura, Nobuya Serino, Motoko Nakajima, Motoki Kitaguchi, Takao Kato, Yo Kawai, Nobuyuki |
| author_facet | Aoyama, Amira Enoto, Teruaki Takahashi, Takuya Watanabe, Sota Takeda, Tomoshi Iwakiri, Wataru Yamasaki, Kaede Iwata, Satoko Ota, Naoyuki Jujo, Arata Tamagawa, Toru Mihara, Tatehiro Hu, Chin-Ping Dohi, Akira Nishimura, Nobuya Serino, Motoko Nakajima, Motoki Kitaguchi, Takao Kato, Yo Kawai, Nobuyuki |
| contents | An uncatalogued bright X-ray transient was detected with MAXI on November 9, 2024, named MAXI J1752$-$457. The NinjaSat X-ray observatory promptly observed the source from November 10 to 18 while the small angular separation from the Sun hampered follow-up campaigns by other X-ray observatories. The MAXI and NinjaSat light curves in the 2-10 keV band showed first and second decaying components at the early and late phases, approximated by exponential functions with e-folding constants of 1.2 $\pm$ 0.2 and 14.9 $\pm$ 0.9 hours (1$σ$ errors), respectively. A single blackbody model reproduces the X-ray spectrum with a softening trend of its temperature decreasing from 1.8 $\pm$ 0.1 keV to 0.59 $\pm$ 0.06 keV. Assuming the unknown source distance at 8 kpc, at which the initial X-ray luminosity roughly corresponds to the Eddington limit, the shrinking blackbody radius was estimated at 5-11 km. This X-ray brightening is interpreted as a superburst in a Galactic low-mass X-ray binary, which is powered by thermonuclear burning triggered presumably by carbon ignition close to the outer crust of the neutron star. The transition between two decaying components occurred at 5.5-7.7 hours, corresponding to the thermal time scale of the burning layer. The ignition column density is estimated to be (2.8-5.1)$\times 10^{12}$ g cm$^{-2}$. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2504_04352 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Thermonuclear superburst of MAXI J1752$-$457 observed with NinjaSat and MAXI Aoyama, Amira Enoto, Teruaki Takahashi, Takuya Watanabe, Sota Takeda, Tomoshi Iwakiri, Wataru Yamasaki, Kaede Iwata, Satoko Ota, Naoyuki Jujo, Arata Tamagawa, Toru Mihara, Tatehiro Hu, Chin-Ping Dohi, Akira Nishimura, Nobuya Serino, Motoko Nakajima, Motoki Kitaguchi, Takao Kato, Yo Kawai, Nobuyuki High Energy Astrophysical Phenomena An uncatalogued bright X-ray transient was detected with MAXI on November 9, 2024, named MAXI J1752$-$457. The NinjaSat X-ray observatory promptly observed the source from November 10 to 18 while the small angular separation from the Sun hampered follow-up campaigns by other X-ray observatories. The MAXI and NinjaSat light curves in the 2-10 keV band showed first and second decaying components at the early and late phases, approximated by exponential functions with e-folding constants of 1.2 $\pm$ 0.2 and 14.9 $\pm$ 0.9 hours (1$σ$ errors), respectively. A single blackbody model reproduces the X-ray spectrum with a softening trend of its temperature decreasing from 1.8 $\pm$ 0.1 keV to 0.59 $\pm$ 0.06 keV. Assuming the unknown source distance at 8 kpc, at which the initial X-ray luminosity roughly corresponds to the Eddington limit, the shrinking blackbody radius was estimated at 5-11 km. This X-ray brightening is interpreted as a superburst in a Galactic low-mass X-ray binary, which is powered by thermonuclear burning triggered presumably by carbon ignition close to the outer crust of the neutron star. The transition between two decaying components occurred at 5.5-7.7 hours, corresponding to the thermal time scale of the burning layer. The ignition column density is estimated to be (2.8-5.1)$\times 10^{12}$ g cm$^{-2}$. |
| title | Thermonuclear superburst of MAXI J1752$-$457 observed with NinjaSat and MAXI |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2504.04352 |