Short gamma-ray bursts (sGRBs) have widely been accepted to arise from a compact object binary merger; neutron star–neutron star or neutron star–black hole. During the merger of a binary neutron star system, magnetic field can be amplified beyond magnetar field strength ($\sim {10}^{15}\text{–}{10}^{16}\text{ G}$) by Kelvin–Helmholtz instabilities. Considering this effect on the GRB “fireball” dynamics, we study the emission, propagation and oscillation of multi MeV–GeV neutrinos through their self-energies and using these we compute the neutrino effective potential up to order $M_W^{-4}$. Additionally, we calculate the number of neutrino events and neutrino flavor ratios that we would expect on Hyper-Kamiokande and DeepCore experiments. We found that MeV neutrinos in a strong magnetic field could provide information of the topology of the field, and that the number of GeV neutrinos expected in DeepCore detector would be directly affected by the strength of the field. It is worth noting that our estimates correspond to the only trustworthy method for verifying the effect of the magnetic field amplification.

短伽玛射线暴（sGRB）是由紧凑的对象二进制合并产生的；中子星-中子星或中子星-黑洞。在双星中子星系统合并期间，磁场可以被放大到超过磁场强度（$〜{10}^{15}\text{–}{10}^{16}\text{ G}$）由开尔文-亥姆霍兹不稳定性。考虑到这种对GRB“火球”动力学的影响，我们研究了多个MeV–GeV中微子通过其自能的发射，传播和振荡，并利用这些自中能计算出中微子有效势。${\mathrm{中号}}_{\mathrm{w\; ^}}^{-4}$。此外，我们计算了在Hyper-Kamiokande和DeepCore实验中所期望的中微子事件和中微子风味比的数量。我们发现强磁场中的MeV中微子可以提供磁场拓扑的信息，而DeepCore检测器中预期的GeV中微子的数量将直接受到磁场强度的影响。值得一提的是，我们的估计值对应于验证磁场放大效果的唯一可信赖的方法。