An axisymmetric magnetohydrodynamic model for the interaction of the solar wind with the local interstellar medium

We numerically analyze a magnetohydrodynamic, steady-state model for the interaction of a spherically symmetric solar wind with a three-component local interstellar medium (LISM), which is composed of plasma, hydrogen atoms, and a magnetic field. The magnetic field is assumed to be parallel to the velocity in the LISM. In this case, the model is axisymmetric. We study the effects of magnetic field on the plasma-flow geometry and on the distribution of hydrogen-atom parameters. In particular, we show that the presence of hydrogen atoms does not affect the qualitative change in the shape of the bow shock, the heliopause, and the solar-wind shock with increasing strength of the interstellar magnetic field. The presence of a magnetic field in the LISM can strongly affect the parameters of the energetic hydrogen atoms originated in the solar wind, although its effect on the “hydrogen wall” observed with the GHRS instrument onboard the HST spacecraft (Linsky and Wood 1996) is marginal.     

Two- and three-dimensional numerical simulations of accretion discs in a close binary system

We perform 2D and 3D numerical simulations of an accretion disc in a close binary system using the simplified flux vector splitting (SFS) finite volume method. In our calculations, the gas is assumed to be ideal with γ =1.01, 1.05, 1.1 and 1.2 . The mass ratio of the mass-losing star to the mass-accreting star is unity. Our results show that spiral shocks are formed on the accretion disc in all cases. In 2D calculations we find that the smaller γ is, the more tightly the spiral winds. We observe this trend in 3D calculations as well in a somewhat weaker sense. Mach numbers in our discs are less than 10. These values are lower than the values in observed accretion discs in close binary systems.
Recently, Steeghs, Harlaftis & Horne found the first convincing evidence for spiral structure in the accretion disc of the eclipsing dwarf nova binary IP Pegasi, using the technique known as Doppler tomography. Although the Mach numbers in present calculations are rather low, we may claim that the spiral structure that we discovered in earlier numerical simulations is now found observationally.     

老虎台矿83001采区电磁辐射规律

以抚顺老虎台矿83001采区煤岩体的电磁辐射为例,分析了采区煤岩体的电磁辐射与应力分布规律,并以此确定了冲击矿压防治的重点区域。      

Effect of Cu toxicity at different salinity on selective group of juvenile pompano Trachinotus ovatus

Effects of copper toxicity and salinity shock on selective group of juvenile pompano Trachinotus ovatus were investigated.The fish were exposed to different Cu2+ concentrations of 0(blank),0.02(C1),0.05(C2),0.10(C3),and 0.15 mg·L–1(C4)at a salinity of 10‰ or 40‰ for 96 h,with the salinity of 29‰ as the control.The results showed that the effects of the acute salinity stimulation to survival rates of pompano between control(29‰)and lower or higher salinity for 96 h were not significant(p0.05).However,the survival rates in each treatment were decreased with the increase of Cu2+ concentration.The dominant factor influencing body moisture of the fish was salinity,and there was no sign that body moisture was correlated with exposure to Cu2+.The gill lamellas in high level of Cu2+ concentration(C4 treatments)were abnormal under the salinity of 40‰ and extremely curly under the salinity of 10‰.Hemorrhage in gill was observed in the two C4 treatments.Under transmission electron microscope,pillar cells in gill lamellas appeared deformed and ruptured in some areas of the epithelia in the higher concentration of Cu2+,resulting in the death of the fish due to the destruction of gill tissue,elevation of the arithmetic mean distance from water to blood,the decrease of oxygen diffusion capacity,and other physiological functions.These findings indicate that the pompano might suffer much more pressure when encountered with Cu2+ pollution and low salinity.     

人工触发闪电连续电流过程与M分量特征

在广州野外雷电试验基地,对2008年和2011年夏季人工触发闪电回击之后的14个连续电流过程和43个M分量的通道底部电流、电场变化和通道亮度进行了同步测量和分析。结果表明:M分量的电流、快慢电场变化和亮度变化波形均近似对称;触发闪电连续电流过程的持续时间、转移电荷量、电流平均值的几何平均值分别为22 ms,6.0 C和273 A;M分量的幅度、转移电荷量、半峰值宽度、上升时间、持续时间的几何平均值分别为409 A,205 mC,520 μs,305 μs和1.6 ms;连续电流持续时间与M分量的个数、相邻M分量之间的时间间隔均存在显著的正相关关系。     

耀斑引发的激波初始速度对激波到达时间预测的影响

利用Hakamada-Akasofu-Fry运动学太阳风模型模拟了1981到1985卡林顿周的48个太阳耀斑事件激发的激波到达地球的时间.结果表明,对模式输入参数之一的激波初始速度进行调整,可以使模拟结果和实际观测基本一致.通过对发生在该时期多个事件的统计分析,分别得到日球表面东、西两半球耀斑爆发对应的激波初始速度调整...     

1604年福建泉州海外地震震级和震源参数的探讨——基于强地震动数值模拟方法

根据历史资料和已有的研究成果,利用两种地震动数值模拟方法对1604年福建泉州海外地震震级和震源参数进行了研究.首先利用经验公式确定了该次地震震级为71/2级和8级时的震源参数,然后基于离散波数法和有限断层地震动随机合成法,并利用基岩与一般场地水平峰值加速度的对应关系,计算了福建沿海8个场点的加速度、速度时程及其峰值,发...     

Two-temperature accretion flows in magnetic cataclysmic variables: structures of post-shock emission regions and X-ray spectroscopy

We use a two-temperature hydrodynamical formulation to determine the temperature and density structures of the post-shock accretion flows in magnetic cataclysmic variables (mCVs) and calculate the corresponding X-ray spectra. The effects of two-temperature flows are significant for systems with a massive white dwarf and a strong white-dwarf magnetic field. Our calculations show that two-temperature flows predict harder keV spectra than one-temperature flows for the same white-dwarf mass and magnetic field. This result is insensitive to whether the electrons and ions have equal temperature at the shock, but depends on the electron–ion exchange rate, relative to the rate of radiative loss along the flow. White-dwarf masses obtained by fitting the X-ray spectra of mCVs using hydrodynamic models including the two-temperature effects will be lower than those obtained using single-temperature models. The bias is more severe for systems with a massive white dwarf.