Dark stars at the Galactic Centre – the main sequence

In regions of very high dark matter density such as the Galactic Centre, the capture and annihilation of WIMP dark matter by stars has the potential to significantly alter their evolution. We describe the dark stellar evolution code D ark S tars , and present a series of detailed grids of WIMP-influenced stellar models for main-sequence stars. We describe the changes in stellar structure and main-sequence evolution which occur as a function of the rate of energy injection by WIMPs, for masses of  0.3–2.0 M_⊙  and metallicities   Z = 0.0003–0.02  . We show what rates of energy injection can be obtained using realistic orbital parameters for stars at the Galactic Centre, including detailed consideration of the velocity and density profiles of dark matter. Capture and annihilation rates are strongly boosted when stars follow elliptical rather than circular orbits. If there is a spike of dark matter induced by the supermassive black hole at the Galactic Centre, single solar mass stars following orbits with periods as long as 50 yr and eccentricities as low as 0.9 could be significantly affected. Binary systems with similar periods about the Galactic Centre could be affected on even less eccentric orbits. The most striking observational effect of this scenario would be the existence of a binary consisting of a low-mass protostar and a higher mass evolved star. The observation of low-mass stars and/or binaries on such orbits would either provide a detection of WIMP dark matter, or place stringent limits on the combination of the WIMP mass, spin-dependent nuclear-scattering cross-section, halo density and velocity distribution near the Galactic Centre. In some cases, the derived limits on the WIMP mass and spin-dependent nuclear-scattering cross-section would be of comparable sensitivity to current direct-detection experiments.     

利用混凝沉淀法处理喷粉工艺中的磷化废水

进行了用混凝沉淀法处理喷粉工艺中磷化废水的试验研究。结果表明,在原水中SS为90-400mg/L,COD为150-400mg/L。在水温15℃、pH为9.0-10.0、搅拌时间为3-5min、PAM投加量为5mg/L/CaCl2投加量为200mg/L的条件下,SS和COD的最大去除率可分别达到90%和75%。     

基于韧性损伤的水下传动装置磨粒磨损与性能退化研究

本文采用基于不可逆热力学原理的韧性金属复杂应力损伤演化模型,对ABAQUS二次开发将损伤模型引入有限元计算,实施含腐蚀传动装置磨粒磨损分析;磨粒-传动轴-配合面耦合模型中,磨粒采用三维球形分形模型,对点蚀和面蚀配合面与磨粒微观接触时损伤演化及传动特性变化进行模拟,发现磨粒挤入配合面后应力三轴度增大,传动轴转动数周后接触面即出现凸峰与沟犁,而且缺陷间存在损伤连通趋势,使结构传动运动能力快速下降;考虑环境温度循环,温度升高使磨粒局部产生应力梯度,对结构传动能力也有不利影响。基于材料损伤演化模型建立细观磨粒磨损与宏观传动装置统一的模拟方法,实现了海洋环境下小间隙配合面磨粒磨损计算,有效预测了传动装置性能退化过程。     

The termination shock in a striped pulsar wind

The origin of radio emission from plerions is considered. Recent observations suggest that radio-emitting electrons are presently accelerated rather than having been injected at early stages of the plerion evolution. The observed flat spectra without a low-frequency cut-off imply an acceleration mechanism that raises the average particle energy by orders of magnitude but leaves most of the particles at an energy of less than approximately a few hundred MeV. It is suggested that annihilation of the alternating magnetic field at the pulsar wind termination shock provides the necessary mechanism. Toroidal stripes of opposite magnetic polarity are formed in the wind emanating from an obliquely rotating pulsar magnetosphere (the striped wind). At the termination shock, the flow compresses and the magnetic field annihilates by driven reconnection. Jump conditions are obtained for the shock in a striped wind. It is shown that the post-shock magnetohydrodynamic parameters of the flow are the same as if the energy of the alternating field had already been converted into plasma energy upstream of the shock. Therefore, the available estimates of the ratio of the Poynting flux to the matter energy flux, σ, should be attributed not to the total upstream Poynting flux but only to that associated with the average magnetic field. A simple model for the particle acceleration in the shocked striped wind is presented.     

Relationship between Composition of Settling Particles and Organic Carbon Flux in the Western North Pacific and the Japan Sea

Settling particles play an important role in transporting organic carbon from the surface to the deep ocean. It is known that major components of settling particles are biogenic silicates (opal), biogenic carbonate (CaCO₃), lithogenic clays and organic matter. Since each component aggregates and/or takes in organic carbon, all of these components have the ability to transport particulate organic carbon (POC) to the interior of the ocean. In this study, sediment trap experiments were carried out in four areas of the western North Pacific (including a marginal sea). Factors are proposed that correlate the composition of settling particles with POC flux. Annual mean organic carbon fluxes at 1 km depth in the western North Pacific Basin, Japan Sea, Hidaka Basin and northern Japan Trench were found to be 14.9, 18.1, 13.0 and 6.6 mg/m²/day, respectively. Organic carbon flux in the western North Pacific was greater than that in the Eastern North Pacific (7.4), the Equatorial Pacific (4.2), the Southern Ocean (5.8) and the Eastern North Atlantic (1.8). In the western North Pacific, it was calculated that 52% of POC was carried by opal particles. Opal is known to be a major component even in the Eastern North Pacific and the Southern Ocean, and the opal fluxes in these areas are similar to those in the western North Pacific. However, the organic carbon flux that was carried by opal particles (OC_opalflux) in the western North Pacific was greater than that in the Eastern North Pacific and the Southern Ocean. These results indicate that the ability of opal particles to transport POC to the deep ocean in the western North Pacific is greater than that in the other areas.     

辽宁冬季城市空气质量分布状况综合研究

利用2006年12月辽宁14个城市的大气环境现状监测资料和沈阳、鞍山、抚顺、本溪4城市可吸收入颗粒物(PM10,PM2.5和PM1)的监测资料,对辽宁冬季各城市的空气质量分布状况进行了综合研究。结果表明:辽宁14个城市的冬季空气质量分布状况为优、良和轻微污染3个等级,其中铁岭、营口和辽阳的空气质量有28 d为良及以上等级;空气质量级别为轻微污染日数最多的城市是本溪,共计12 d;其次是葫芦岛、沈阳、鞍山、抚顺、盘锦、阜新,共计7—10 d。各城市的首要污染物是PM10。由于冬季燃煤量的增加,沈阳、鞍山、抚顺和本溪4城市PM2.5日平均浓度值的超标率为77.4%—90.3%。     

乌鲁木齐河源1号冰川不溶微粒的季节变化特征

冰芯中的不溶微粒是反映大气粉尘的良好指标,亦是冰芯定年的重要方法。为了探究不溶微粒在雪层中的季节变化特征,对采自乌鲁木齐河源1号冰川4 130 m处的雪冰样品进行不溶微粒分析。表层雪中粗微粒浓度在一年中有2个峰值,分别出现在12~3月、6~9月;总微粒只有一个峰值区,出现在4~8月。对比同期气象资料发现,其受降水、大气环流以及局地风影响显著。结合雪层物理剖面和微粒在雪层中的浓度发现：污化层是粗颗粒（直径大于10 μm）聚集的区域。对该粒径范围的微粒浓度峰值进行跟踪,发现不溶微粒在雪层中的浓度和位置变化与融水、物理成冰过程密切相关。     

Organic geochemical characteristics of time-series settling particles in northern South China Sea and their implications

Organic carbon, total nitrogen, amino acids, sugars, and chlorophyll were determined in < 1 mm fractions of the samples collected by successive large aperture time-series sediment traps (Honjo-Mark M) in northern South China Sea during September 1987 to October 1988. The ratio of C/N and the relative abundance of amino acids and sugars show that organic matter in the settling particles from northern South China Sea is derived mainly from marine plantkon (especially phytoplankton). The organic carbon fluxes in our sediment traps are lower than those in other sediment traps. But the relative contents of C_org/total particulate matter are generally similar to those in the Panama Basin, Arabian Sea and Subarctic Pacific. It is suggested that monsoon-caused changes of physical and chemical conditions in the upper euphotic layer would control the fluxes of organic matter as well as its composition and transport in northern South China Sea. This project was financially supported by both Sino-German Scientific Cooperation Program and National Natural Science Foundation of China (No. 49070269, 49776297).     

Using X‐ray observations to identify the particle acceleration mechanisms in VHE SNRs and “dark” VHE sources

Very high energy (VHE) γ‐ray observations have proven to be very successful in localizing Galactic acceleration sites of VHE particles. Observations of shell‐type supernova remnants have confirmed that particles are accelerated to VHE energies in supernova blast waves; the interpretation of the γ‐ray data in terms of hadronic or leptonic particle components in these objects relies nevertheless strongly on input from X‐ray observations. The largest identified Galactic VHE source class consists of pulsar wind nebulae, as detected in X‐rays. Many of the remaining VHE sources remain however unidentified until now. With X‐ray observations of these enigmatic “dark” objects one hopes to solve the following questions: What is the astrophysical nature of these sources? Are they predominantly electron or hadron accelerators? And what is their contribution to the overall cosmic ray energy budget? The paper aims to provide an overview over the identification status of the Galactic VHE source population. (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)