论文标题
改进的Lemaitre-Tolman模型以及星系组的质量和转弯半径II：暗能量的作用
Improved Lemaitre-Tolman model and the mass and turn-around radius in group of galaxies II: the role of dark energy
论文作者
论文摘要
在本文中，我们在Lemaitre-Tolman（LT）模型上扩展了先前的研究\ cite {delpopolo2021}，以显示模型的预测在修改了状态参数（$ w $）时的预测如何变化。在先前的研究中，被认为仅由宇宙常数构成暗能量。在本文中，如先前的研究一样，我们还考虑了角动量和动力摩擦（$jη$ lt模型）的效果，该效果修改了扰动的演变，最初是随着哈勃流动而移动的。作为解决运动方程式的第一步，我们计算了质量，$ m $和转弯半径，$ r_0 $之间的关系。如果一个人知道转向半径$ r_0 $的值，则可以获得研究对象的质量。作为第二步，我们像上一篇论文一样建立了速度，$ v $和radius，$ r $之间的关系。该关系适合组和集群的数据。由于关系$ v-r $取决于哈勃常数和对象的质量，因此我们获得了研究对象的两个参数的优化值。比较$jη$ lt结果（$ W = -1 $）和情况$ W = -1/3 $的质量减少25 \％，而Hubble常数从$ W = -1 $增加到$ W = -1/3 $。最后，所获得的质量，$ m $和$ r_0 $的质量值可以对状态参数的暗能量方程（$ w $）构成约束。
In this paper, we extend our previous study \cite{DelPopolo2021} on the Lemaitre-Tolman (LT) model showing how the prediction of the model changes when the equation of state parameter ($w$) of dark energy is modified. In the previous study, it was considered that dark energy was merely constituted by the cosmological constant. In this paper, as in the previous study, we also took into account the effect of angular momentum and dynamical friction ($Jη$ LT model) that modifies the evolution of a perturbation, initially moving with the Hubble flow. As a first step, solving the equation of motion, we calculated the relationship between mass, $M$, and the turn-around radius, $R_0$. If one knows the value of the turn-around radius $R_0$, it is possible to obtain the mass of the studied objects. As a second step, we build up, as in the previous paper, a relationship between the velocity, $v$, and radius, $R$. The relation was fitted to data of groups and clusters. Since the relationship $v-R$ depends on the Hubble constant and the mass of the object, we obtained optimized values of the two parameters of the objects studied. The mass decreases of a factor of maximum 25\% comparing the $Jη$ LT results (for which $w=-1$) and the case $w=-1/3$, while the Hubble constant increases going from $w=-1$ to $w=-1/3$. Finally, the obtained values of the mass, $M$, and $R_0$ of the studied objects can put constraints to the dark energy equation of state parameter, $w$.
