论文标题
中子星的内部加热机制
Internal heating mechanisms in neutron stars
论文作者
论文摘要
中子星的冷却（以下简称NS）有可能揭示超密集物质的重要特征。它们的表面温度以$ \ leq 10^{6} \，{\ it {yr}} $的公平样本而闻名，除了标准冷却机制（Neutrino+Photon发射而无需内部热量），可以容纳一些例外。但是，对于较旧的物体，必须考虑一些内部加热以解释表面温度高于预期的温度。我们在本文中重新审视了费米克暗物质，旋转化学加热和磁场衰减的动力学加热。我们发现，NS比$ \ sim 10^{6} \，{\ it {yr}} $可以解释，但是较老的``黑色寡妇''系统比这三种机制所预测的值要热得多，这是指尚不清楚的旧NS的尚不清楚的加热因子。
The cooling of neutron stars (hereafter NS) has the potential to reveal important features of superdense matter. Their surface temperatures are known for a fair sample of NS with ages $\leq 10^{6} \, {\it{yr}}$, and with a few exceptions, can be accommodated by standard cooling mechanisms (neutrino+photon emission without internal heating). However, for the older objects it is necessary to consider some internal heating to explain surface temperatures higher than expected. We revisit in this paper the kinetic heating by fermionic dark matter, rotochemical heating and magnetic field decay. We found that NS slightly older than $\sim 10^{6} \, {\it{yr}}$ can be explained by them, but the older ``black widow'' systems are much hotter than the values predicted by these three mechanisms, pointing towards a yet unknown heating factor for old NS.
