Spherical Collapse(球形塌陷)研究综述
Spherical Collapse 球形塌陷 - We perform extensive nonlinear numerical simulations of the spherical collapse of (charged) wavepackets onto a charged black hole within Einstein-Maxwell theory and in Einstein-Maxwellscalar theory featuring nonminimal couplings and a spontaneous scalarization mechanism. [1] The simplest models of dark matter halo formation rely on the heuristic assumption, motivated by spherical collapse, that virialized haloes originate from initial regions that are maxima of the smoothed matter density field. [2] Here, we give an explicit integral solution, utilizing methods recently applied to the “geometric goat problem” and to the dynamics of spherical collapse. [3] We find that the Rastall parameter affects crucially the dynamics of density contrasts for DM and DE and the fate of spherical collapse is different in comparison to the case of general relativity (GR). [4] This paper investigates the dynamics of spherical collapse in the framework of energy–momentum squared gravity. [5] We analyzed the nonspherical collapse, coalescence, and breakup of bubbles in a megasonic field using a compressible, locally homogeneous model of a gas-liquid two-phase medium. [6] This allows the determination of the time for quasi-spherical collapse, which is shown to happen generically earlier than in the spherical case. [7] We test our method within the Zel'dovich approximation, presenting also an analytic solution including tidal fields and spherical collapse on small scales. [8]我们在爱因斯坦-麦克斯韦理论和以非最小耦合和自发标量化机制为特征的爱因斯坦-麦克斯韦标量理论中，对（带电）波包在带电黑洞上的球面坍缩进行了广泛的非线性数值模拟。 [1] 最简单的暗物质晕形成模型依赖于由球形坍缩推动的启发式假设，即虚拟化晕起源于平滑物质密度场最大值的初始区域。 [2] 在这里，我们利用最近应用于“几何山羊问题”和球形坍塌动力学的方法，给出了一个显式积分解。 [3] 我们发现，Rastall 参数对 DM 和 DE 的密度对比动力学产生了至关重要的影响，并且与广义相对论 (GR) 的情况相比，球形坍塌的命运是不同的。 [4] 本文研究了能量-动量平方重力框架下球形坍塌的动力学。 [5] 我们使用气液两相介质的可压缩局部均匀模型分析了兆声波场中气泡的非球形坍塌、聚结和破裂。 [6] 这允许确定准球形塌陷的时间，这通常比球形情况更早发生。 [7] 我们在 Zel'dovich 近似中测试我们的方法，还提出了一个解析解，包括小尺度的潮汐场和球形塌陷。 [8]
spherical collapse model 球形塌陷模型
We compared the mass distribution in the CB with predictions from the spherical collapse model and analysed the acceleration field in the CB. [1] A self-similar spherical collapse model predicts a dark matter (DM) splashback and accretion shock in the outskirts of galaxy clusters while misses a key ingredient of structure formation – processes associated with mergers. [2] Here we investigate how dark energy can affect the growth of large scale structures of the universe in framework of spherical collapse model. [3] By using the spherical collapse model, we investigate the growth of perturbations in time varying $G$ cosmologies. [4] We use N-body simulations to examine whether a characteristic turnaround radius, as predicted from the spherical collapse model in a $\rm {\Lambda CDM}$ Universe, can be meaningfully identified for galaxy clusters, in the presence of full three-dimensional effects. [5]我们将 CB 中的质量分布与球形坍塌模型的预测进行了比较，并分析了 CB 中的加速度场。 [1] 一个自相似的球形坍缩模型预测了星系团外围的暗物质 (DM) 溅射和吸积冲击，而忽略了结构形成的一个关键因素——与合并相关的过程。 [2] 在这里，我们在球形坍塌模型的框架下研究暗能量如何影响宇宙大尺度结构的生长。 [3] 通过使用球形塌陷模型，我们研究了随时间变化 $G$ 的扰动增长 宇宙学。 [4] 我们使用 N 体模拟来检查在存在完整三维的情况下，是否可以从 $\rm {\Lambda CDM}$ 宇宙中的球形坍塌模型预测的特征周转半径为星系团有意义地识别效果。 [5]
spherical collapse calculation
We compare the median of this stochastic map with spherical collapse calculations and discuss challenges involved in modeling the evolution of the density field on these scales. [1] We present a halo mass function accurate over the full relevant Hu-Sawicki $f(R)$ parameter space based on spherical collapse calculations and calibrated to a suite of modified gravity $N$-body simulations that include massive neutrinos. [2]我们将这个随机地图的中值与球形坍塌计算进行比较，并讨论在这些尺度上模拟密度场演变所涉及的挑战。 [1] 我们基于球形坍缩计算提出了一个在整个相关 Hu-Sawicki $f(R)$ 参数空间上精确的光环质量函数，并校准到一套改进的重力 $N$-body 模拟，其中包括大量中微子。 [2]