arXiv 0802.11772008-02-21hep-ph

了解更多关于从银河系超新星的中微子观测中可以得出的结论

Learning more about what can be concluded from the observation of neutrinos from a galactic supernova

Solveig Skadhauge, Renata Zukanovich Funchal

备注：: 17 pages. References added and updated, additions in acknowledgment

摘要：

我们调查什么人可以希望了解的参数，描述的银河系超新星爆炸所发射的中微子通量使用的观测兆吨级的水切伦科夫探测器。我们计算允许的区域，可以通过拟合这些参数，以模拟观察事件，这样的检测器。所有四个可用的检测通道（逆β衰变、氧上的电荷和中性电流以及电子上的弹性散射）都包括在拟合中，并且我们使用十维参数空间。九个参数描述了初始中微子通量，被称为超新星参数。此外，我们还考虑了中微子在超新星外层的物质效应对中微子的依赖性，即对中微子与超新星的混合角$θ_{13}$的依赖性。如果我们不做任何额外的假设，这些参数，我们表明，人们可以希望确定$θ_{13}$相当不错，而除了参数描述的$\barν_e$流量，大多数超新星参数是相当困难的约束，即使四个检测通道可以完全分离。

英文摘要：

We investigate what one can hope to learn about the parameters that describe the neutrino fluxes emitted by the explosion of a galactic supernova using the observations of a megaton-size Water-Cherenkov detector. We calculate the allowed regions that can be obtained by fitting these parameters to a simulated observation of events by such a detector. All four available detection channels (inverse beta decay, charge and neutral current on oxygen and elastic scattering on electrons) are included in the fit and we use a ten dimensional parameters space. Nine parameters describe the initial neutrino fluxes and are referred to as the supernova parameters. Furthermore, we include the dependence on the Chooz mixing angle $θ_{13}$, which controls the matter effects that the neutrino undergoes in the outer-parts of the supernova. If we do not make any extra assumption on these parameters, we show that one can hope to determine $θ_{13}$ quite well whereas, except for the parameters describing the $\barν_e$ flux, most of the supernova parameters are rather difficult to constrain, even if the four detection channels could be completely separated.

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