球形坍缩模型的一些改进
Some improvements to the spherical collapse model
摘要：
我研究的联合效应的动力学摩擦，潮汐扭矩和宇宙学常数对星系团的形成我表明，在高密度的环境中，如丰富的星系团，动力学摩擦和潮汐扭矩减缓崩溃的低？峰值在微扰的坍缩时间中产生可观察到的变化，并且因此，与坍缩的微扰绑定的质量减少。此外，相对于经典的球形模型，坍缩的延迟产生较不致密的区域吸积较少质量的趋势，诱导过密区域向更高质量的偏置，我展示了如果动力学摩擦，考虑了潮汐力矩和非零宇宙学常数的影响，并采用扩展的PressSchecter（EPS）方法计算了质量函数的影响。我比较了Reed等人（2003）中给出的数值质量函数利用本文得到的理论质量函数，我证明了本文得到的势垒相对于其他先前模型更好地描述了质量函数的演化（Sheth & Tormen 1999，MNRAS，308，119（以下简称ST）; Sheth & Tormen 2002，MNRAS，329，61（以下简称ST 1））
英文摘要：
I study the joint effect of dynamical friction, tidal torques and cosmological constant on clusters of galaxies formation I show that within high-density environments, such as rich clusters of galaxies, both dynamical friction and tidal torques slows down the collapse of low-? peaks producing an observable variation in the time of collapse of the perturbation and, as a consequence, a reduction in the mass bound to the collapsed perturbation Moreover, the delay of the collapse produces a tendency for less dense regions to accrete less mass, with respect to a classical spherical model, inducing a biasing of over-dense regions toward higher mass I show how the threshold of collapse is modified if dynamical friction, tidal torques and a non-zero cosmological constant are taken into account and I use the Extended Press Schecter (EPS) approach to calculate the effects on the mass function Then, I compare the numerical mass function given in Reed et al (2003) with the theoretical mass function obtained in the present paper I show that the barrier obtained in the present paper gives rise to a better description of the mass function evolution with respect to other previous models (Sheth & Tormen 1999, MNRAS, 308, 119 (hereafter ST); Sheth & Tormen 2002, MNRAS, 329, 61 (hereafter ST1))
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