论文标题
在状态方程内具有诱导表面张力的状态方程
Neutron star cooling within the equation of state with induced surface tension
论文作者
论文摘要
我们研究了在状态方程中描述的中性星的热演化，并具有诱导的表面张力（IST），该表面张力（IST）重现了正常核物质的特性，满足质子流量约束，提供了对在核核碰撞实验过程中产生的强子多重性的高质量描述，并且与Sattrophysical观察和GW17的构造同样兼容。该型号具有强大的直接URCA进程，适用于高于$ 1.91〜M _ {\ odot} $的恒星。即使没有引入核配对，状态的IST方程与可用的冷却数据也非常吻合。我们还分析了单线质子/中子和三元中子配对对不同质量中子星的冷却的影响。我们表明，在Cassiopeia a中心对紧凑物体的描述不一定需要包括中子超流体和/或质子超导性。我们的结果表明，Cassiopeia a的数据可以通过$ 1.66〜m _ {\ odot} $ star充分重现，并具有光元素的气氛。此外，IST EOS通过快速冷却的$ \ sim $ \ sim $ \ sim $ 1.955〜m _ {\ odot} $ star带有配对和不成熟的物质或以$ 1.91〜m _ {\ odot} $ 1.91〜m _ {\ odot} $ sath in Neutimon和pottion in Neutnon和pottion in Neutnon和pottion andron和pottion andron in Neutnon和pottion netron和pottion andron和pottion，IST EOS可以通过快速冷却的Cassiopeia a的观测数据集来复制Cassiopeia a的表面温度。
We study the thermal evolution of neutron stars described within the equation of state with induced surface tension (IST) that reproduces properties of normal nuclear matter, fulfills the proton flow constraint, provides a high-quality description of hadron multiplicities created during the nuclear-nuclear collision experiments, and it is equally compatible with the constraints from astrophysical observations and the GW170817 event. The model features strong direct Urca processes for the stars above $1.91~M_{\odot}$. The IST equation of state shows very good agreement with the available cooling data, even without introducing nuclear pairing. We also analysed the effect of the singlet proton/neutron and triplet neutron pairing on the cooling of neutron stars of different mass. We show that the description of the compact object in the center of the Cassiopeia A does not necessarily require an inclusion of neutron superfluidity and/or proton superconductivity. Our results indicate that data of Cassiopeia A can be adequately well reproduced by a $1.66~M_{\odot}$ star with an atmosphere of light elements. Moreover, the IST EoS reproduces each of the observational datasets for the surface temperature of Cassiopeia A either by a rapidly cooling $\sim$ $1.955~M_{\odot}$ star with paired and unpaired matter or by a $1.91~M_{\odot}$ star with the inclusion of neutron and proton pairings in the singlet channel.
