Thermonuclear Superburst of MAXI J1752−457 Observed with NinjaSat and MAXI

Amira Aoyama, Teruaki Enoto, Takuya Takahashi, Sota Watanabe, Tomoshi Takeda, Wataru Iwakiri, Kaede Yamasaki, Satoko Iwata, Naoyuki Ota, Arata Jujo, Toru Tamagawa, Tatehiro Mihara, Chin-Ping Hu, Akira Dohi, Nobuya Nishimura, Motoko Serino, Motoki Nakajima, Takao Kitaguchi, Yo Kato, Nobuyuki Kawai and (NinjaSat collaboration)
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Abstract

An uncatalogued bright X-ray transient was detected with MAXI on 2024 November 9, 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 ± 0.2 and 14.9 ± 0.9 hr (1σ errors), respectively. A single blackbody model reproduces the X-ray spectrum with a softening trend of its temperature decreasing from 1.8 ± 0.1 keV to 0.59 ± 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 hr, corresponding to the thermal timescale of the burning layer. The ignition column density is estimated to be (1.8–2.8) × 1012 g cm−2.
用NinjaSat和MAXI观测到的MAXI J1752−457热核超爆
MAXI于2024年11月9日探测到一个未编目的明亮x射线瞬变,命名为MAXI J1752−457。从11月10日到18日,NinjaSat x射线天文台迅速观测到了该源,而与太阳的小角度分离阻碍了其他x射线天文台的后续活动。MAXI和NinjaSat在2-10 keV波段的光曲线显示出第一和第二衰减分量,分别以指数函数表示,e折叠常数分别为1.2±0.2和14.9±0.9 hr (1σ误差)。单黑体模型再现了x射线光谱,其温度从1.8±0.1 keV降至0.59±0.06 keV,呈现出软化趋势。假设未知源距离为8kpc,初始x射线光度大致与Eddington极限相对应,则黑体半径估计为5-11 km。这种x射线变亮被解释为银河系低质量x射线双星中的一次超级爆发,它是由热核燃烧提供动力的,可能是由中子星外壳附近的碳点火引发的。两个衰变组分之间的转变发生在5.5 ~ 7.7 hr,对应于燃烧层的热时间尺度。点火柱密度估计为(1.8-2.8)× 1012 g cm−2。
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