ausblenden:
Schlagwörter:
Astrophysics, High Energy Astrophysical Phenomena, astro-ph.HE,Nuclear Theory, nucl-th
Zusammenfassung:
Very recently, it has been shown that there is an upper bound on the squared
sound speed of nuclear matter from the transport, which reads $c_{\rm s}^2 \leq
0.781$. In this work, we demonstrate that this upper bound is corroborated by
the reconstructed equation of state (EOS; modeled with a nonparametric method)
for ultradense matter. The reconstruction integrates multimessenger observation
for neutron stars, in particular, the latest radius measurements for PSR
J0437-4715 ($11.36^{+0.95}_{-0.63}$ km), PSR J0030+0451
($11.71^{+0.88}_{-0.83}$ km, in the ST+PDT model), and PSR J0740+6620
($12.49^{+1.28}_{-0.88}$ km) by NICER have been adopted. The result shows in
all cases, the $c_{\rm s}^2 \leq 0.781$ upper limit for EOS will naturally
yield the properties of matter near the center of the massive neutron star
consistent with the causality-driven constraint from pQCD, where, in practice,
the density in implementing the pQCD likelihood ($n_{\rm L}$) is applied at
$10n_s$ (where $n_s$ is the nuclear saturation density). We also note that
there is a strong correlation for the maximum $c_s^2$ with $n_{\rm L}$, and
$c_{\rm s}^2 \leq 0.781$ is somehow violated when $n_{\rm L} = n_{\rm c,TOV}$.
The result indicates that a higher $n_{\rm L}$, even considering the
uncertainties from statistics, is more natural. Moreover, the remarkable
agreement between the outcomes derived from these two distinct and independent
constraints (i.e., the transport calculation and pQCD boundary) lends strong
support to their validity. In addition, the latest joint constraint for
$R_{1.4}$, $R_{2.0}$, $R_{1.4}-R_{2.0}$, and $M_{\rm TOV}$ are
$11.94_{-0.68}^{+0.77}$ km, $11.99_{-0.67}^{+0.88}$ km, $-0.1_{-0.27}^{+0.42}$
km, and $2.24_{-0.10}^{+0.13}M_\odot$ (at $90\%$ credible level), respectively.
