A five-wave Harten–Lax–van Leer Riemann solver for relativistic magnetohydrodynamics

We present a five-wave Riemann solver for the equations of ideal relativistic magneto-hydrodynamics. Our solver can be regarded as a relativistic extension of the five-wave HLLD Riemann solver initially developed by Miyoshi & Kusano for the equations of ideal magnetohydrodynamics. The solution to the Riemann problem is approximated by a five-wave pattern, comprising two outermost fast shocks, two rotational discontinuities and a contact surface in the middle. The proposed scheme is considerably more elaborate than in the classical case since the normal velocity is no longer constant across the rotational modes. Still, proper closure to the Rankine–Hugoniot jump conditions can be attained by solving a non-linear scalar equation in the total pressure variable which, for the chosen configuration, has to be constant over the whole Riemann fan. The accuracy of the new Riemann solver is validated against one-dimensional tests and multidimensional applications. It is shown that our new solver considerably improves over the popular Harten–Lax–van Leer solver or the recently proposed HLLC schemes.     

Emission and cooling by CO in interstellar shock waves

We have calculated emission by CO molecules from interstellar shock waves. Two approximations have been used to determine the population densities,   n_J   , of the rotational levels, J : steady state  (∂/∂ t ≡ 0)  and statistical equilibrium  (d/d t ≡ 0)  . A large-velocity-gradient approximation to the line-transfer problem was adopted in both cases. We find that there can be substantial differences between the values of the integrated rotational line intensities calculated in steady state and in the limit of statistical equilibrium. On the other hand, although CO can be the dominant coolant towards the rear of the cooling flow which follows the dynamical heating of the gas, the rate of cooling computed assuming statistical equilibrium is likely to be reasonably accurate, given that the limit of statistical equilibrium is approached in this region.     

冲击变质陨石橄榄石晶内高压多形转变特征与条件

对2个不同冲击变质程度球粒陨石研究表明,橄榄石晶内高压多形转变可在较低温度(<1000℃)和较大压力范围内(14.5～23GPa)产生。橄榄石晶内高压相转变主要是形成薄层状林伍德石,不发生直接的橄榄石-瓦士利石转变。由微晶集合体组成的薄层状林伍德石多沿着橄榄石中层错和面状裂隙分布并替代母相橄榄石。某些陨石中橄榄石产出薄层状瓦士利石和薄层状林伍德石组合,这些瓦士利石的形成与退变质作用有关,是压力释放过程林伍德石被瓦士利石替代的结果。研究结果对探讨岩石圈俯冲板块橄榄石多形转变环境和温度压力条件具有一定的参考意义。     

四川汶川Ms 8 级地震触发的典型滑坡的风险指标反演

2008年汶川大地震触发了数以万计的崩塌和滑坡,特别是沿发震断裂分布一系列大型的高速远程滑坡。为了探索地震诱发大型高速远程滑坡运动速度的反演方法,以汶川大地震典型高速远程滑坡为例,在野外调查和室内分析的基础上,结合前人的研究成果,对沿映秀－北川断裂展布的5个典型滑坡的速度进行了反演和计算。结果表明,5个滑坡的最大速度均大于50m/s,其中大光包滑坡速度最大,其下部滑体的最大速度约为300m/s,上部滑体凌空飞行的初速度高达165.6 m/s。同时,对上述滑坡的视摩擦系数进行了计算,4个滑坡的视摩擦系数介于0.16~0.4之间。这一研究的目的在于为类似地区地震滑坡的速度、最大位移量的预测和风险评估提供基础数据,对于类似地区的防灾减灾具有一定的参考价值。     

星际无碰撞激波的Balmer双线结构

Balmer发射线是研究星际无碰撞激波物理性质的重要途径之一.星际无碰撞激波的Balmer发射线包括宽线和窄线两个明显的成分.通常认为,这种双线成分是与激波联系在一起的,宽线产生于激波前慢中性粒子与激波后高能质子的电荷交换,反映了激波后粒子的热运动状况,而窄线则产生于激波前慢中性粒子的激发,反映了激波前粒子的热运动状况.但是,近来更细致的观测和理论计算表明,超新星遗迹中Balmer发射线的双线结构很可能还要受到其他因素的影响,并且与激波速度和电子-质子的热平衡有着密切的关系.该文将讨论影响Balmer双线结构的各种因素,并讨论Balmer双线结构在超新星遗迹研究中的一些应用.     

Revealing the “fingerprints” of the magnetic precursor of C-shocks

We present the first C-shock and radiative transfer model that calculates the evolution of the line profiles of neutral and ion species like SiO, H¹³CO⁺ and HN¹³C for different flow times along the propagation of the shock through the unperturbed gas. We find that the line profiles of SiO characteristic of the magnetic precursor stage have very narrow linewidths and are centered at velocities close to the ambient cloud velocity, as observed toward the young shocks in the L1448-mm outflow. Consistently with previous works, our model also reproduces the broad SiO emission detected in the high velocity gas in this outflow, for the downstream postshock gas in the shock. This implies that the different velocity components observed in L1448-mm are due to the coexistence of different shocks at different evolutionary stages.     

Location of the bow shock and ion composition boundaries at Venus—initial determinations from Venus Express ASPERA-4

For the first time since 1992 when the Pioneer Venus Orbiter (PVO) ceased to operate, there is again a plasma instrument in orbit around Venus, namely the ASPERA-4 flown on Venus Express (inserted into an elliptical polar orbit about the planet on April 11, 2006). In this paper we report on measurements made by the ion and electron sensors of ASPERA-4 during their first five months of operation and, thereby, determine the locations of both the Venus bow shock (BS) and the ion composition boundary (ICB) under solar minimum conditions. In contrast to previous studies based on PVO data, we employ a 3-parameter fit to achieve a realistic shape for the BS. We use a different technique to fit the ICB because this latter boundary cannot be represented by a conic section. Additionally we investigate the dependence of the location of the BS on solar wind ram pressure (based on ASPERA-4 solar wind data) and solar EUV flux (using a proxy from Earth).     

汤坑井水位观测系统体应变响应分析

井水位观测系统作为一种天然的体应变计,我们可以把固体潮理论值作为观测井的输入值,以维尼迪可夫调和分析结果的半日波M2波群的振幅比作为井水位观测系统的灵敏度,其倒数即为观测格值,然后就可将井水位观测转换成体应变值。本文以汤坑井为例,计算分析了由印尼远震、汶川地震、台湾地震共三种地震类型对汤坑井水位所激励的水震波,结果显示,所记录到的水震波是叠加在体应变固体潮背景上的一种阶跃,对三种地震类型都分别做出了不同程度的响应,体应变固体潮响应幅度最高可达10^-7,体应变响应幅度与地震能量成正比,响应延迟时间与震中距成正比。     

赤点石斑鱼HSP60基因克隆及弧菌应激前后的组织表达特性分析

HSP60(heat shock protein 60,热休克蛋白60)作为高度保守的热休克蛋白家族的一员,不仅可以在应激状态下帮助其他蛋白正确折叠并恢复天然构象,还可作为危险信号作用于天然免疫系统.基于HSP60的EST序列设计特异引物,采用RACE技术成功克隆获得赤点石斑鱼HSP60 cDNA全序列及基因组全序列....     

中微子泄漏与超新星爆发

在超新星爆发过程中,中微子的泄漏非常重要.采用一维球对称模型,在不同的中微子泄漏模式下,数值模拟了质量为12 M_⊙、14 M_⊙及15 M_⊙的Ⅱ型超新星爆发过程.结果表明:不同的中微子泄漏模式对超新星塌缩、激波的传播和爆发都具有影响;并给出了最有利于Ⅱ型超新星爆发的相关参数的最佳值.此外还讨论了物态方程与压缩模量对模拟结果的影响.