The special GRB 130310A was observed by Fermi Gamma-Ray Burst Monitor and Large Area Telescope, with T ₉₀∼ 2.4 s. With a combination of a Band function and a blackbody (BB) function, the time-resolved spectral analysis of GRB 130310A confirmed that there is a sub-dominate thermal component in the early period (e.g., slice T ₀ + [4.03 – 4.14] s) spectrum with BB temperature (kT) being ∼7∼5 keV, which can be interpreted as photosphere emission. The precursor of GRB 130310A can be fitted well with a BB component with kT ∼ 45 keV, which is higher than that of the main burst. It suggests that the radiation of GRB 130310A is in transition from thermal to non-thermal. Such a transition is an indication of the change in jet composition from a fireball to a Poynting-flux-dominated jet. A very high peak energy is obtained in the first time bin, with the peak energy E_p of the Band component for Band+BB and Band model being ∼8.5∼5.2 MeV and ∼11.1∼7.4 MeV, respectively. Afterwards, the E_p drops to ∼ 1 MeV. The E_p evolution patterns with respect to the pulses in the GRB 130310A light curves show a hard-to-soft evolution. The interpretation of the high peak energy E_p within the photosphere and internal shock model is difficult. It also suggests that at least for some bursts, the Band component must invoke a non-thermal origin in the optically thin region of a GRB outflow. Assuming the redshift is z ∼ 0.1 ∼ 8, the radius of the jet base r ₀ ∼ 10⁹ cm to allow (1 + σ ₁₅) > 1 in line with the calculation results of the magnetization parameter at ∼10¹⁵ cm (σ ₁₅). However, the value of (1 + σ ₁₅) is ≃ 1 in the zone z around 3 for r ₀ ∼ 10⁹ cm, suggesting the non-excluded possibility that the origin is from ICMART with a low value. The photosphere-internal shock seems capable of interpreting the high peak energy, which requires electron Lorentz factor γ_e ∼ 60 and ε_e ∼ 0.06.

费米伽马暴监测器和大面积望远镜观测到特殊的GRB 130310A ， T ₉₀ ∼ 2.4 s。结合波段函数和黑体 (BB) 函数，GRB 130310A 的时间分辨光谱分析证实，在早期存在次主导热分量（例如，切片T ₀ + [4.03 – 4.14] s）BB温度（kT）为~7~5 keV的光谱，可以解释为光球发射。GRB 130310A的前身可以很好地与具有kT的BB组件配合∼ 45 keV，高于主爆发。这表明 GRB 130310A 的辐射正在从热辐射到非热辐射。这种转变表明射流成分从火球到以坡印廷通量为主的射流发生了变化。在第一次 bin 中获得了非常高的峰值能量，Band+BB 和 Band 模型的 Band 分量的峰值能量E _p 分别为~8.5~5.2 MeV 和~11.1~7.4 MeV。之后，E _p 下降到 ∼ 1 MeV。GRB 130310A 光变曲线中与脉冲有关的E _{p演变模式显示出从硬到软的演变。} 高峰值能量E _p的解释 光球内和内部冲击模型是困难的。它还表明，至少对于某些爆发，波段分量必须在 GRB 流出的光学薄区域中调用非热源。假设红移为z ∼ 0.1 ∼ 8，则射流基部半径r ₀ ∼ 10 ⁹ cm 允许(1 + σ ₁₅ ) > 1 符合磁化参数在∼10 ¹⁵ cm ( σ ₁₅的计算结果）。然而，在r ₀ ∼ 10 ^9的区域z中，(1 + σ ₁₅ ) 的值是 ≃ 1 在3 附近 cm，表明来源来自ICMART的低值的非排除可能性。光球内激波似乎能够解释高峰值能量，这需要电子洛伦兹因子γ _e ∼ 60 和ε _e ∼ 0.06。