arXiv 1405.68732014-05hep-ph

仙后座A中中子星的轴子质量极限

Axion mass limit from observations of the neutron star in Cassiopeia A

Lev B. Leinson

备注：: 10 pages, 1 figure
发表信息：: J. Cosmol. Astropart. Phys. 08 (2014) 031
DOI：: 10.1088/1475-7516/2014/08/031

摘要：

钱德拉直接观测仙后座A（Cas A NS）中孤立的中子星的表面温度，最近几个科学小组同时提出了它的冷却方案，对超流中子星核心的未知性质提出了严格的限制。还发现，Cas A NS的热能损失比中微子发射所能解释的强度大大约两倍。我们使用这些独特的数据和定义良好的冷却方案来估计KSVZ轴子与中子相互作用的强度。我们推测中子星超流核的轴子发射是导致能量损失增大的原因。如果轴子和中微子的损失是可比的，我们发现$c_{n}^{2}m_{a}^{2}\sim 5.7\times 10^{-6}\,\text{eV}^2$，其中$m_{a}$是轴子质量，$c_{n}$是中子的有效佩切-奎因电荷。（考虑到强子轴子模型的QCD不确定性，无量纲常数$c_{n}$的范围可以从$-0.05$到$ 0.14$。）

英文摘要：

Direct Chandra observations of a surface temperature of isolated neutron star in Cassiopeia A (Cas A NS) and its cooling scenario which has been recently simultaneously suggested by several scientific teams put stringent constraints on poorly known properties of the superfluid neutron star core. It was found also that the thermal energy losses from Cas A NS are approximately twice more intensive than it can be explained by the neutrino emission. We use these unique data and well-defined cooling scenario to estimate the strength of KSVZ axion interactions with neutrons. We speculate that enlarged energy losses occur owing to emission of axions from superfluid core of the neutron star. If the axion and neutrino losses are comparable we find $c_{n}^{2}m_{a}^{2}\sim 5.7\times 10^{-6}\,\text{eV}^2$, where $m_{a}$ is the axion mass, and $c_{n}$ is the effective Peccei-Quinn charge of the neutron. (Given the QCD uncertainties of the hadronic axion models, the dimensionless constant $c_{n}$ could range from $-0.05$ to $ 0.14$.)

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