Long duration gamma-ray bursts (GRBs) are among the least understood astrophysical transients powering the high-energy universe. To date, various mechanisms have been proposed to explain the observed electromagnetic GRB emission. In this work, we show that, although different jet models may be equally successful in fitting the observed electromagnetic spectral energy distributions, the neutrino production strongly depends on the adopted emission and dissipation model. To this purpose, we compute the neutrino production for a benchmark high-luminosity GRB in the internal shock model, including a dissipative photosphere as well as three emission components, in the jet model invoking internal-collision-induced magnetic reconnection and turbulence (ICMART), in the case of a magnetic jet with gradual dissipation, and in a jet with dominant proton synchrotron radiation. We find that the expected neutrino fluence can vary up to three orders of magnitude in amplitude and peak at energies ranging from 10⁴ to 10⁸ GeV. For our benchmark input parameters, none of the explored GRB models is excluded by the targeted searches carried out by the IceCube and ANTARES Collaborations. However, our work highlights the potential of high-energy neutrinos of pinpointing the underlying GRB emission mechanism and the importance of relying on different jet models for unbiased stacking searches.

持续时间较长的伽马射线暴 (GRB) 是为高能宇宙提供动力的最不为人知的天体物理瞬变之一。迄今为止，已经提出了各种机制来解释观察到的电磁 GRB 发射。在这项工作中，我们表明，尽管不同的射流模型在拟合观测到的电磁光谱能量分布方面可能同样成功，但中微子的产生很大程度上取决于所采用的发射和耗散模型。为此，我们计算了内部激波模型中基准高光度 GRB 的中微子产生，包括耗散光球层和三个发射分量，在调用内部碰撞诱导磁重联和湍流 (ICMART) 的喷射模型中，在磁射流逐渐消散的情况下，在质子同步辐射占主导地位的射流中。我们发现预期的中微子注量在能量范围从 10⁴到 10 ⁸ GeV。对于我们的基准输入参数，IceCube 和 ANTARES Collaborations 进行的目标搜索没有排除任何探索过的 GRB 模型。然而，我们的工作强调了高能中微子在确定潜在 GRB 发射机制方面的潜力，以及依赖不同射流模型进行无偏叠加搜索的重要性。