论文标题
在非常庞大的中子星的最小半径上
On the minimum radius of very massive neutron stars
论文作者
论文摘要
Prospects of establishing the radii of massive neutron stars in PSR J1614-2230 and PSR J0740+6620 from NICER and Chandra observatories hold the potential to constrain the equation of state (EoS) of matter to densities well beyond those encountered in canonical stars of mass $\sim 1.4\,{\rm M}_{\odot}$.在这项工作中，我们研究了由密集物质EOSS支持的非常庞大的中子星的半径，直至最大质量，$ m _ {\ rm max} $。具有宽容物质的模型的结果与包括一阶强体到Quark相变的模型形成鲜明对比。我们发现，在$ m _ {\ rm max} $上的下限上有一个上限，上面的巨大脉冲星的半径是排除太软夸克，并且上限上的上限$ m _ {\ rm max} $，在大型脉冲星的半径上，在巨大的脉冲中，巨大的脉搏偏向于过渡到过渡到过于建立的低调，而又高低了。还简要讨论了Inspiral二进制中子星的未来重力波事件的半径推论所起的互补作用。
Prospects of establishing the radii of massive neutron stars in PSR J1614-2230 and PSR J0740+6620 from NICER and Chandra observatories hold the potential to constrain the equation of state (EoS) of matter to densities well beyond those encountered in canonical stars of mass $\sim 1.4\,{\rm M}_{\odot}$. In this work, we investigate the relation between the radii of very massive neutron stars up to the maximum mass, $M_{\rm max}$, supported by dense matter EoSs. Results from models with hadronic matter are contrasted with those that include a first-order hadron-to-quark phase transition. We find that a lower bound on $M_{\rm max}$ with an upper bound on the radius of massive pulsars serves to rule out too soft quark matter, and an upper bound on $M_{\rm max}$ with a lower bound on the radius of massive pulsars strongly disfavors a transition into too-stiff quark matter appearing at low densities. The complementary role played by radius inferences from future gravitational wave events of inspiraling binary neutron stars is also briefly discussed.
