论文标题
超新星中微子的总能量以及中子星的潮汐变形和结合能
Total Energy in Supernova Neutrinos and the Tidal Deformability and Binding Energy of Neutron Stars
论文作者
论文摘要
超新星中微子辐射的能量是一种基本量，与中子恒星的重力结合能密切相关。最近，中子星的潮汐变形性受重力波观测的限制。通过考虑几个状态方程，我们发现潮汐变形性与中子星的结合能之间存在很强的相关性。我们使用这种相关性来增强对中子星和超新星中中微子能量的结合能的预测。我们找到了在$ \ sim1.5 \ times 10^{53} $ ergs的超新星中形成的中子星的最小结合能。如果超新星中的中微子能显着低于此值，则强烈表明新的未观察到的颗粒正在携带一些超新星能。或者，如果在$ \ sim 6 \ sim 6 \ times 10^{53} $ ergs上观察到中微子能量，它将很大程度上暗示形成（也许令人惊讶的）大型中子星。
The energy radiated in supernova neutrinos is a fundamental quantity that is closely related to the gravitational binding energy of a neutron star. Recently the tidal deformability of neutron stars was constrained by gravitational wave observations. By considering several equations of state, we find a strong correlation between the tidal deformability and neutron star binding energy. We use this correlation to sharpen predictions of the binding energy of neutron stars and the total neutrino energy in supernovae. We find a minimum binding energy for a neutron star formed in a supernova of $\sim1.5\times 10^{53}$ ergs. Should the neutrino energy in a supernova be significantly below this value, it would strongly suggest new unobserved particles are carrying away some of the supernova energy. Alternatively, if the neutrino energy is observed above $\sim 6\times 10^{53}$ ergs, it would strongly imply the formation of a (perhaps surprisingly) massive neutron star.
