GRB 210610B: The Internal and External Plateau As Evidence For The Delayed Outflow Of Magnetar

Yining Wei, Xianggao Wang, Da-Bin Lin, Weikang Zheng, Liang-Jun Chen, Sheng-Yu Yan, Shuangxi Yi, Qi Wang, ZI-Min Zhou, Hui-Ya Liu, En-Wei Liang
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Abstract

After launching a jet, outflows of magnetar were used to account for the achromatic plateau of afterglow and the early X-ray flux plateau known as "internal plateau''. The lack of detecting magnetic dipole emission together with the energy injection feature in a single observation poses confusion until the long gamma-ray burst (GRB) 210610B is detected. GRB 210610B is presented with an optical bump following an early X-ray plateau during the afterglow phase. The plateau followed by a steep decline flux overlays in the steadily decaying X-ray flux with index α X,1 ∼ 2.06, indicating an internal origin and that can be fitted by the spin-down luminosity law with the initial plateau luminosity log10 L X ∼ 48.29 erg s-1 and the characteristic spin-down timescale T ∼ 2818 s. A subsequent bump begins at ∼ 4000 s in R band with a rising index α R,1 ∼ -0.30 and peaks at ∼ 14125 s, after which a decay index α R,2 ∼ 0.87 and finally transiting to a steep decay with α R,3 ∼ 1.77 achieve the closure relation of the external shock for the normal decay phase as well as the magnetar spin-down energy injection phase, provided that the average value of the photon index Γγ = 1.80 derived from the spectral energy distributions (SEDs) between the X-ray and optical afterglow. The closure relation also works for the late X-ray flux. Akin to the traditional picture of GRB, the outflow powers the early X-ray plateau by dissipating energy internally and collides with the leading decelerating blast burst as time goes on, which could interpret the exotic feature of GRB 210610B. We carry out a Markov Chain Monte Carlo (MCMC) simulation and obtain a set of best parameters: ε B ≈ 4.2 × 10-5, ε e ≈ 0.16, E K,iso ≈ 4.2× 1053 ergs, Γ0 ≈ 851, A* ≈ 0.11, L inj,0 ≈ 2.31 × 1050 erg s-1. The artificial light curve can fit the afterglow data well. After that, we estimated the average Lorentz factor and the X-ray radiation efficiency of the later ejecta are 35 and 0.13%, respectively.
GRB 210610B:内部和外部高原是磁星延迟外流的证据
在发射喷流之后,磁星的外流被用来解释余辉的消色高原和被称为 "内部高原 "的早期 X 射线通量高原。在探测到长伽马射线暴(GRB)210610B 之前,由于在一次观测中没有探测到磁偶极子发射和能量注入特征,因此造成了混淆。GRB 210610B 在余辉阶段的早期 X 射线高原之后出现了一个光学凸起。高原之后的通量急剧下降,与指数 α X,1 ∼ 2.06 的稳定衰减 X 射线通量重叠,表明其内部起源,可以用自旋下降光度定律来拟合,初始高原光度 log10 L X ∼ 48.随后在 R 波段从 ∼ 4000 秒开始出现凸起,指数 α R,1 ∼ -0.之后衰变指数α R,2 ∼ 0.87,最后过渡到α R,3 ∼ 1.77的陡峭衰变,从而实现了正常衰变阶段以及磁星自旋下降能量注入阶段的外部冲击闭合关系,条件是根据X射线和光学余辉之间的光谱能量分布(SED)得出的光子指数Γγ = 1.80的平均值。闭合关系也适用于晚期 X 射线通量。与GRB的传统图景相似,流出物通过内部耗散能量为早期X射线高原提供能量,并随着时间的推移与前导减速爆炸爆发相撞,这可以解释GRB 210610B的奇异特征。我们进行了马尔可夫链蒙特卡罗(MCMC)模拟,得到了一组最佳参数:ε B ≈ 4.2 × 10-5,ε e ≈ 0.16,E K,iso ≈ 4.2× 1053 ergs,Γ0 ≈ 851,A* ≈ 0.11,L inj,0 ≈ 2.31 × 1050 erg s-1。人工光曲线可以很好地拟合余辉数据。之后,我们估算出后期喷出物的平均洛伦兹因子和 X 射线辐射效率分别为 35% 和 0.13%。
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