论文标题
通过低质量中子星星质学估计核饱和参数
Estimating the nuclear saturation parameter via low-mass neutron star asteroseismology
论文作者
论文摘要
我们检查了来自感冒中子恒星的重力波中的基本压力（$ f $ - ）和第一压力（$ p_1 $ - ）模式频率，这些星星由各种统一的现实状态方程式构建。通过计算出的频率，我们根据恒星平均密度和参数（$η$）的平方根的函数来得出$ f $ - 和$ p_1 $ -mode频率，$ f_f $和$ f_f $和$ f_f $和$ f_f $和$ f_f $和$ f_f $和$ f_f $和$ f_f $和$ f_f $和$ f_f $和$ f_f $和$ f_f $）的经验公式的组合。借助我们的经验公式，我们表明，通过同时观察$ f $ - 和$ p_1 $ - mmode重力波，当$ 1.5 \ lyssim f_ {p_1}/f_1}/f_f \ lyssim 2.5 $（与$ \\ lyssim 0.9m $ $ simpiationdy sim simpiationdy sim sim prodiationdy sim portiational sim simpiationdy sim prodiatiate youth $ odot $ odot youth $ odot youth $ odot） 10 \％$准确性，这对中子恒星物质的EOS有很大限制。此外，我们发现最大$ f $ mmode频率与中子星的最小半径密切相关。也就是说，如果人们观察到$ f $ mode的频率较大，则可能会限制最小中子星半径的上限。
We examine the fundamental ($f$-) and the 1st pressure ($p_1$-) mode frequencies in gravitational waves from cold neutron stars constructed with various unified realistic equations of state. With the calculated frequencies, we derive the empirical formulae for the $f$- and $p_1$-mode frequencies, $f_f$ and $f_{p_1}$, as a function of the square root of the stellar average density and the parameter ($η$), which is a combination of the nuclear saturation parameters. With our empirical formulae, we show that by simultaneously observing the $f$- and $p_1$-mode gravitational waves, when $1.5\lesssim f_{p_1}/f_f\lesssim 2.5$ (which corresponds to neutron star models with the mass of $\lesssim 0.9M_\odot$), one could estimate the value of $η$ within $\sim 10\%$ accuracy, which makes a strong constraint on the EOS for neutron star matter. In addition, we find that the maximum $f$-mode frequency is strongly associated with the minimum radius of neutron star. That is, if one would observe a larger frequency of the $f$-mode, one might constrain the upper limit of the minimum neutron star radius.
