通过$Z^\prime$介导的中微子加热为伽马射线暴提供能量
Energizing gamma ray bursts via $Z^\prime$ mediated neutrino heating
AI总结：
本文通过扩展标准模型引入 $U(1)_{\rm{B-L}}$ 规范群，利用 $Z^\prime$ 规范玻色子介导中微子对湮灭增强 GRB 能量沉积，并从观测能量中获得强于散射实验的规范耦合约束。
摘要：
中微子的对湮灭（$ν\overlineν\rightarrow e^+e^-$）能够为剧烈的恒星爆炸（如伽马射线暴（GRBs））提供能量。通过修改牛顿时空的背景时空，这种中微子加热机制中的能量可以进一步增强。然而，在牛顿背景或 Schwarzschild 和 Hartle-Thorne 背景下，均无法达到 GRB 的最大能量（$\sim 10^{52}~\rm{erg}$）。另一方面，使用修改引力理论或 Quintessence 场作为背景几何，则可以达到 GRB 的最大能量。在本文中，我们考虑通过一个额外的 $U(1)_{\rm{B-L}}$ 规范群来扩展标准模型，并增加中微子对湮灭过程中的能量沉积，其中包含了由属于该模型的 $Z^\prime$ 规范玻色子介导的贡献。从观测到的 GRB 能量中，我们获得了不同背景时空下对 $U(1)_{\rm{B-L}}$ 规范耦合的约束。我们发现，在小规范玻色子质量极限下，修改引力理论和 Quintessence 背景下的规范耦合界限强于来自中微子-电子散射实验的界限。未来精度更高的 GRB 观测可以进一步加强这些界限。
英文摘要：
The pair annihilation of neutrinos $(ν\overlineν\rightarrow e^+e^-)$ can energize violent stellar explosions such as gamma ray bursts (GRBs). The energy in this neutrino heating mechanism can be further enhanced by modifying the background spacetime over that of Newtonian spacetime. However, one cannot attain the maximum GRB energy $(\sim 10^{52}~\rm{erg})$ in either the Newtonian background or Schwarzschild and Hartle-Thorne background. On the other hand, using modified gravity theories or the Quintessence field as background geometries, the maximum GRB energy can be reached. In this paper, we consider extending the standard model by an extra $U(1)_{\rm{B-L}}$ gauge group and augmenting the energy deposition by neutrino pair annihilation process including contributions mediated by the $Z^\prime$ gauge boson belonging to this model. From the observed energy of GRB, we obtain constraints on $U(1)_{\rm{B-L}}$ gauge coupling in different background spacetimes. We find that the bounds on gauge coupling in modified gravity theories and quintessence background are stronger than those coming from the neutrino-electron scattering experiments in the limit of small gauge boson masses. Future GRB observations with better accuracy can further strengthen these bounds.
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