2024/07/16 by Wenjie Zhou, Zhou, Wenjie, Hong Shen +5
Physics and Astronomy · Earth and Planetary Sciences · Engineering · #Pulsars and Gravitational Waves Research #Geophysics and Gravity Measurements #Inertial Sensor and Navigation
paper · pdf · doi:10.48550/arxiv.2407.11447
This study investigates the first-order phase transition within neutron stars, leveraging the deep neural network (DNN) framework alongside contemporary astronomical measurements. The equation of state (EOS) for neutron stars is delineated in a piecewise polytropic form, with the speed of sound (cs) serving as a pivotal determinant. In the phase transition region, cs is presumed to be zero, while in other intervals, it is optimized utilizing the DNN. Various onset energy densities of phase transition (εpt), spanning from 2ε0 to 3ε0 (where ε0 denotes the energy density at nuclear saturation density), as well as phase transition widths (Δε) ranging from 0.5ε0 to ε0, are examined. Our findings underscore that smaller values of εpt lead to a more substantial impact of Δε on neutron star properties, encompassing maximum mass, corresponding radius, tidal deformability, phase transition mass, and trace anomaly. Conversely, when εpt exceeds 2.5ε0, the influence of Δε diminishes, resulting in a stiffer EOS compared to scenarios lacking a phase transition. Furthermore, the trace anomaly at high density shifts to negative values upon the commencement of the phase transition. It is noteworthy that the correlations between the average speed of sound at different energy density segments demonstrate a notably weak connection. The discernment of whether a phase transition has occurred with the present observables of neutron stars poses a challenging task.