论文标题
在海王星大气中观察银河中微子的概念研究
Concept Study for Observing Galactic Neutrinos in Neptune's Atmosphere
论文作者
论文摘要
我讨论了利用冰巨头作为银河中微子的目标的概念性空间中微子检测器的可行性。这项研究的目的源于希望找到一种新方法来观察银河系的银河系核（GC）和超大质量黑洞SAG a*。除了光密度太密集而无法探测的空间区域外，已经对GC进行了观察。在这些地区，我们可以使用中微子。来自活性银河核的中微子在极端的能量下排放，10 GEV至EEV尺度，但在地球上测得的通量极低。诸如Icecube天文台之类的中微子望远镜只能测量可能与GC相关的少数中微子。但是使用引力镜头，我们的太阳可以用作镜头，将中微子的“光”收集能力提高了$ 10^{13} $，而权衡了最低焦点位于22 au。这意味着天王星和海王星是这些中微子与轨道上的中微子相互作用并观察到轨道上中微子的作用的合适自然靶标。初步研究使用CERN开发的粒子物理模拟工具箱Geant4来促进通过海王星大气的能量颗粒的传播。研究各个方面以了解这些粒子相互作用的行为。对于这些方面的每个方面，我们都会修改几个变量，例如粒子类型，能量，相互作用深度和距表面的轨道距离。我还讨论了这种中微子检测器的多功能性，该中微子检测器有可能绘制冰巨头的内部结构，对来自GC的中微子的深入研究，以及将此方法用于其他宇宙中微子来源的可能性。
I discuss the feasibility of a conceptual space-based neutrino detector that utilizes the Ice Giants as Targets for Galactic Neutrinos. The purpose of this research stems from the concept of wanting to find a new method of observing the Galactic Core (GC) of the Milky Way and the Supermassive black hole, Sag A*. Observations of the GC have been made in every accessible wavelength except for the regions of space that are too dense for photons to probe. In these regions, we may instead use neutrinos. Neutrinos from the Active Galactic Nucleus are emitted at extreme energies, 10 GeV to EeV scales, but have an extremely low flux measured here at Earth. Neutrino telescopes such as the IceCube Observatory have only been able to measure a handful of neutrinos that might correlate to the GC. But using Gravitational lensing, our sun can be used as a lens which increases the 'light' collection power for neutrinos by a factor of $10^{13}$, with the trade-off that the minimum focal point is located at 22 AU. This means that Uranus and Neptune are suitable natural targets for these neutrinos to interact with and observe the effects of a spacecraft in orbit. Initial studies use GEANT4, a particle physics simulation toolbox developed by CERN, to facilitate the propagation of energetic particles passing through the atmosphere of Neptune. Various aspects are studied to understand the behaviors of these particle interactions. For each of these aspects, we modify several variables such as particle type, energy, interaction depth, and orbital distance from the surface. I also discuss the versatility of this neutrino detector which has the possibility of mapping out the inner structure of the Ice Giants, in-depth studies of the neutrinos coming from the GC, and possibilities to use this method for other cosmic neutrino sources.
