Entropy change and phase transitions in an expanding Universe

The work compiles a correlated study of a gravitational quasi equilibrium thermodynamic approach for establishing and signifying a unique behavior of the cosmological entropy and phase transitions in an expanding Universe. On the basis of prescribed boundary conditions for the cluster temperature a relation for the intra‐cluster medium (ICM) of galaxy clusters has been derived. A more productive and signifying approach of the correlation functions used for galaxy clustering phenomena shows a unique behavior of the entropy change where a phenomenon known as the gravitational phase transition occurs. This unique behavior occurs with a symmetry breaking from mild clustering to low clustering and from mild clustering to high clustering which differs from a normal symmetry breaking in material sciences. We also derive results for the specific latent heat associated with the phase transitions of 3.20 T_c and 0.55 T_c for the mildly clustered phase to the low clustered phase and from the mildly clustered phase to the highly clustered phase, respectively. (© 2015 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

相对密实度对含黏粒砂土动剪切模量与阻尼比影响的试验研究

利用GCTS共振柱系统开展一系列含黏粒砂土的动力特性试验,研究相对密实度对含黏粒砂土动剪切模量和阻尼比的影响,并探讨其影响规律。试验结果表明:相对密实度对动剪切模量、动剪切模量比、阻尼比、最大动剪切模量均有影响。动剪切模量随着相对密实度的增加而变大,但动剪切模量增大的幅度更大;当黏粒含量较小时,动剪切模量比随相对密实度的增加而变大,当黏粒含量较高(≥16%)时,相对密实度对动剪切模量比基本没有影响。阻尼比随相对密实度的增加逐渐变小;最大动剪切模量随相对密实度的增加而增大,但黏粒含量不同,其最大动剪切模量增大幅度不同,同时建立最大动剪切模量随相对密实度变化的关系式,并给出相关参数。     

Structure and kinematics of the interstellar medium around WR 142a: Searching for traces of the action of stellar wind

Based on our Hα interferometric observations and CO data, we analyze the structure and kinematics of the gas in an extended region of the Cygnus arm around the recently discovered star WR 142a. We have established that WR 142a and the ionized hydrogen in its immediate neighborhood are associated with the complex of molecular clouds observed in a region with l ～ 78°–80°30′, b ～ 2°–3°20′, and V _LSR ～ 4–16 km s^?1. Traces of the action of the stellar wind from WR 142a on the ambient gas have been found to the northeast of the star in a region devoid of dense absorbing foreground clouds. These include very weak thin gas and dust filaments as well as high-velocity components of the Hα profile, which can be interpreted as a possible expansion of the shell swept up by the wind with a velocity as high as 50–80 km s^?1. Giant regions of reduced CO emission dominated by high-velocity motions of ionized hydrogen have been detected. Stars of the Cyg OB2 association and the cluster NGC 6910 can be responsible for these motions.     

塔克拉玛干沙漠荒漠过渡带春季风沙活动特征——以肖塘为例

 通过对沙尘暴强化观测试验期间风速、跃移颗粒数、输沙量等资料的统计与计算,对塔克拉玛干沙漠北缘荒漠过渡带肖塘地区春季风沙活动进行了研究。结果表明,肖塘地区春季2 m高度1 s时距的起沙风速为4.9～5.0 m·s-1,1 min时距的起沙风速为4.4 m·s-1;起沙风速随着风速等级的增加,出现的频率相应减少,主要集中在4.4～8.4 m·s-1 之间;输沙势、输沙量的方位分布与起沙风相似,以ENE、E和ESE 3个方位为主,观测期间（1个月）总输沙势为80.8 VU,合成输沙势为13.7 VU,合成输沙势方向为241°;最大可能输沙总量为1 921.8 kg·m-1,合成输沙量为286.8 kg·m-1,合成输沙方向为235°,与输沙势的合成方向一致。     

新月形沙丘表面100cm高度内风沙流输沙量垂直分布函数分段拟合

为研究新月形沙丘表面不同层位风沙流输沙量的垂直分布函数,实测了塔克拉玛干沙漠腹地典型新月形沙丘表面100 cm高度内(以1 cm分隔)的输沙量。分段拟合分析表明:新月形沙丘迎风坡脚输沙量垂直分布规律不完全服从指数函数,出现与戈壁风沙流结构特征相似的"象鼻效应",在0~3 cm区间内输沙量逐渐增大,3cm以上输沙量随高度呈指数函数衰减;沙丘顶部0~10 cm区间输沙量随高度呈指数函数衰减,10 cm以上呈二次函数衰减;沙丘左翼端输沙量随高度呈幂函数分布,沙丘右翼端0~20 cm内以指数函数衰减,20 cm以上呈三次函数衰减;沙丘背风坡脚风沙流输沙量在0~60 cm和60 cm以上分别呈不同形式的三次函数分布。     

晚更新世以来闽东南老红砂沉积粒度特征与古气候变化

对闽东南深沪湾老红砂风沙沉积进行粒度测试,提取对环境变化敏感的粒级组分,结合年代学数据,初步划分了研究区晚更新世中晚期以来的气候变化阶段和气候驱动因素。研究发现,研究区经历了较冷干-暖湿-冷干-暖湿4个气候变化过程。气候变化主要受控于太阳辐射,表现出明显的23 ka长岁差周期、14.2 ka、11.8 ka半岁差周期,叠加约0.25 ka的双世纪周期,陆地-海洋-大气系统的内部因素对表现出来的百年周期可能产生放大或缩小影响。70.8—46.4 ka BP和21.3—11.6 ka BP两个阶段老红砂沉积速率较大,是老红砂风沙堆积的两个主要时期,两个阶段沉积速率分别达到30 mm/(100 a)、650 mm/(100 a)。     

Overall efficiency of a V-shaped nylon net fence in preventing sand damage to the Mogao Grottoes

A V-shaped nylon net fence installed in 1990 on top of the Mogao Grottoes is shown to be effectively resisting aeolian sand damage to the grottoes. The structure guides and causes deposition of sand from westerly wind (the primary hard wind), but to some extent hinders the inverse function of easterly wind carrying sand away from the grottoes toward Mount Mingsha. The gobi side by the fence experiences higher wind speed, so that on which are easily formed undercutting pits, and the deposited sands on it generally form double-peak structures due to abundant sand sources. If the earth surface characteristics in gobi areas by both sides of the fence are quite varied, the erosion and deposition features of the accumulating sand section are similar in different seasons; however, if the earth surface characteristics are similar, the features become irregular in different seasons. Sand depositions with long slope feet are formed along the south and north sides of V-shaped nylon net fence. Disrupted by strong westerly wind and northwesterly wind, sand accumulations by north of the fence are in form of single peaks. Although the operation duration of the V-shaped nylon net fence has exceeded its design life (10 years), our observations indicate that it is still effective in reducing wind-driven sand damages to the Mogao Grottoes, so it should not be withdrawn.     

Sound waves in the intracluster medium

We present an analysis of the behaviour of a perturbed radio cocoon. Comparisons with observations of sound waves detected in the Perseus and Virgo clusters suggest the separations of observed ripples correspond to the natural oscillation frequency of the cocoon. An energy injection rate consistent with active galactic nucleus power is required to offset the strong acoustic damping of cocoon oscillations, suggesting the sources are in equilibrium with the intracluster medium (ICM), and the oscillations are effectively undamped. Viscous dissipation of sound waves provides ICM heating that can quench cooling flows on time-scales greatly exceeding the oscillation time-scale. Thermal conductivity is likely to be heavily suppressed.