再考虑中子星核心中电磁碰撞引起的中微子对轫致辐射
Neutrino pair bremsstrahlung due to electromagnetic collisions in neutron star cores revisited
AI总结：
研究中子星核心中电磁碰撞引起中微子对轫致辐射的机制，发现非超导物质中该过程不重要，而超导物质中轻子碰撞贡献残余中微子发射。
摘要：
我们重新考虑中子星核心中核子（npeμ）中带电粒子电磁碰撞引起的中微子对轫致辐射发射问题。考虑了两种极限情况：（i）质子处于正常态，（ii）质子处于超导态。在两种情况下，轫致辐射发射率Q^em_Br的主要贡献来自介质中电磁相互作用的横向部分。对于非超导物质，由于等离子体屏蔽在横向通道中的动态特性，我们得到一个不寻常的Q^em_Br比例于T^{23/3}的温度依赖性，但其值比以前的研究要小得多，使该过程在实践中变得不重要。相反，在超导和超流物质中，涉及核子的中微子发射过程被抑制，而由轻子碰撞引起的轫致辐射则为中子星核心物质的中微子发射率提供残余贡献。在超导情况下，等离子体屏蔽变得静态，标准的Q^em_Br比例于T^8的温度缩放得以恢复。给出了两种极限情况下的Q^em_Br的简单解析表达式。
英文摘要：
We reconsider the problem of neutrino pair bremsstrahlung emission originating from the electromagnetic collisions of charged particles in nucleonic ($npeμ$) neutron star cores. Two limiting cases are considered: (i) protons are in the normal state and (ii) protons are in the superconducting state. In both cases, the dominant contribution to the bremsstrahlung emissivity $Q^{\mathrm{em}}_{\mathrm{Br}}$ comes from the transverse part of in-medium electromagnetic interactions. For non-superconducting matter, we obtain an unusual $Q^{\mathrm{em}}_{\mathrm{Br}}\propto T^{23/3}$ temperature dependence due to the dynamical character of plasma screening in the transverse channel, but considerably smaller values of $Q^{\mathrm{em}}_{\mathrm{Br}}$ than in previous studies, rendering the considered process unimportant in practice. In contrast, for superconducting and superfluid matter, the neutrino emission processes involving nucleons are suppressed and $Q^{\mathrm{em}}_{\mathrm{Br}}$ due to lepton collisions provides the residual contribution to the neutrino emissivity of neutron star core matter. In the superconducting case, the plasma screening becomes static and the standard $Q^{\mathrm{em}}_{\mathrm{Br}}\propto T^{8}$ temperature scaling is restored. Simple analytical expressions for $Q^{\mathrm{em}}_{\mathrm{Br}}$ in both limiting cases are provided.
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