The effect of metallicity on the minimum mass ratio of W Ursae Majoris-type systems

According to the prevenient theoretical study, the minimum mass ratio for tidal stability of W Ursae Majoris (W UMa) systems is q _min?=(M ₂/M ₁)～0.071–0.078. However, the mass ratios of some observed W UMa binaries are smaller than the theoretical minimum mass ratio. Using Eggleton’s stellar evolution code, we study the effects of metallicity and evolution on the minimum mass ratio of W UMa systems (M ₁=1.2M _⊙). We assume that $k_{1}^{2}=k_{2}^{2}$ for the component’s dimensionless gyration radii and that the contact degree is about 70 per cent. We find that the dynamical stability of W UMa binaries depends on the metallicity of W UMa systems. For the W UMa systems at age = 0 Gyr, the distribution of the minimum mass ratio has a fairly wide range, from 0.083 to 0.064, with the metallicity range from Z=0.0001 to 0.03. W UMa systems with Z=0.01 have the smallest value of the minimum mass ratio, which is about 0.064. The existence of low-q systems can be explained partly by the dependence of the dimensionless gyration radius on the metallicity. In addition, the dependence of the minimum mass ratio on the evolution, as suggested by previously work, is confirmed.     

Contribution of close double white dwarfs to the Galactic gravitational wave foreground

This paper provides new detailed specifics and characteristics of the close double white dwarfs (CDWDs) LISA foreground noise floor using the newest information on the astrophysics with binary population algorithms, which were judged to satisfy the observations. We use the binary population synthesis approach of CDWDs in combination with the latest findings of synthesis models from Han (Mon. Not. R. Astron. Soc. 296:1019, 1998), here, specifically formation by the three evolutionary channels of (a) stable Roche lobe overflow plus common envelope (RLOF?+?CE), (b) CE plus CE, (c) exposed core plus CE. We collect resulting CDWDs in the frequency range of 10^?8 Hz to 10^?2 Hz and compare strength and number statistics per resolvable frequency bin to derive the properties of the noise floor and the nature of possible outliers that may become individually resolvable. We find resolvable outliers to be solely produced by CE?+?CE evolution; the other two channels contribute only to the unresolvable foreground noise. Within the CE?+?CE evolution a detailed look into the chemical buildup of the stars reveals dominantly double helium (He?+?He) WDs or carbon-oxygen CO?+?He WDs.     

The light-weighted age and metallicity of Galactic globular clusters

Spectra synthesis is entering a new era with the availability of large and high-quality spectroscopic data and full spectrum fitting methods. Establishing the reliability whether the STARLIGHT code (a full spectrum fitting code, Cid Fernandes et al. (Mon. Not. R. Astron. Soc. 358:363, 2005)) is suitable to study the properties of various types of galaxies is vital to galaxy study. In testing this possibility, Galactic globular clusters (GCs) provide an excellent medium. Taking the 40 Galactic GCs as an example in our work, we analyze their integrated spectra from Schiavon et al. (Astrophys. J. Suppl. 160:163, 2005) and obtain their mixtures of stellar populations that best represents their composite nature. Through analyzing the distributions of stellar ages and metallicities respectively, we find that the stellar metallicity distribution is centered at a low value and the stellar age distribution is very scattered. To compare with the literature, we also calculate the light-weighted ages and metallicities of GCs, and we find that the light-weighted metallicities agree with the literature, while the light-weighted ages are lower than those of the literature. This demonstrates that STARLIGHT can be used to obtain the metallicities of GCs.     

Habitable zones and UV habitable zones around host stars

Ultraviolet radiation is a double-edged sword to life. If it is too strong, the terrestrial biological systems will be damaged. And if it is too weak, the synthesis of many biochemical compounds cannot go along. We try to obtain the continuous ultraviolet habitable zones, and compare the ultraviolet habitable zones with the habitable zones of host stars. Using the boundary ultraviolet radiation of ultraviolet habitable zone, we calculate the ultraviolet habitable zones of host stars with masses from 0.08 to 4.00 M _⊙. For the host stars with effective temperatures lower than 4,600 K, the ultraviolet habitable zones are closer than the habitable zones. For the host stars with effective temperatures higher than 7,137 K, the ultraviolet habitable zones are farther than the habitable zones. For a hot subdwarf as a host star, the distance of the ultraviolet habitable zone is about ten times more than that of the habitable zone, which is not suitable for the existence of life.     

Coupled convection and tidal dissipation in Europa’s ice shell

We performed 2D numerical simulations of oscillatory tidal flexing to study the interrelationship between tidal dissipation (calculated using the Maxwell model) and a heterogeneous temperature structure in Europa’s ice shell. Our 2D simulations show that, if the temperature is spatially uniform, the tidal dissipation rate peaks when the Maxwell time is close to the tidal period, consistent with previous studies. The tidal dissipation rate in a convective plume encased in a different background temperature depends on both the plume and background temperature. At a fixed background temperature, the dissipation increases strongly with plume temperature at low temperatures, peaks, and then decreases with temperature near the melting point when a melting-temperature viscosity of 10¹³ Pa s is used; however, the peak occurs at significantly higher temperature in this heterogeneous case than in a homogeneous medium for equivalent rheology. For constant plume temperature, the dissipation rate in a plume decreases as the surrounding temperature increases; plumes that are warmer than their surroundings can exhibit enhanced heating not only relative to their surroundings but relative to the Maxwell-model prediction for a homogeneous medium at the plume temperature. These results have important implications for thermal feedbacks in Europa’s ice shell.To self-consistently determine how convection interacts with tidal heating that is correctly calculated from the time-evolving heterogeneous temperature field, we coupled viscoelastic simulations of oscillatory tidal flexing (using Tekton) to long-term simulations of the convective evolution (using ConMan). Our simulations show that the tidal dissipation rate resulting from heterogeneous temperature can have a strong impact on thermal convection in Europa’s ice shell. Temperatures within upwelling plumes are greatly enhanced and can reach the melting temperature under plausible tidal-flexing amplitude for Europa. A pre-existing fracture zone (at least 6 km deep) promotes the concentration of tidal dissipation (up to ∼20 times more than that in the surroundings), leading to lithospheric thinning. This supports the idea that spatially variable tidal dissipation could lead locally to high temperatures, partial melting, and play an important role in the formation of ridges, chaos, or other features.     

Zn2+对日本沼虾(Macrobrachium nipponensis)的急性致毒效应

在水温(27.4±1.3)℃条件下,以体长(33.23±1.66)mm、体质量(0.7893±0.1518)g的日本沼虾为实验动物,采用静水停食法开展了Zn2+对日本沼虾的急性毒性实验,并以此为基础,测定了Zn2+不同质量浓度水平下日本沼虾的耗氧率与窒息点.结果表明:(1)Zn2+对日本沼虾的急性致死效应与其呼吸生理代谢受阻密切相关;(2) Zn2+对日本沼虾24h、48h、72h、96h的半致死质量浓度依次为1.493、0.844、0.643和0.464mg/L; (3) Zn2+对日本沼虾昼均、夜均和日均耗氧率均无显著影响的阈值为0.046mg/L,该值为Zn2+对日本沼虾急性毒性的安全质量浓度;(4) Zn2+对日本沼虾产生轻度胁迫和中度胁迫的质量浓度范围分别为0.046-0.064mg/L和0.064-0.082mg/L.     

陆相盆地古生产力研究现状

古生产力是指地质历史时期生物在能量循环过程中固定能量的速率。陆相盆地古生产力的研究包括古生产力的大小及其组成研究两个方面。目前主要通过有机碳、生物硅和生物标志化合物等指标来评估陆相盆地古生产力的大小;通过生物标志化合物指标,包括正烷烃、萜类、甾类分子标志化合物等指标来研究陆相盆地古生产力的组成。陆相盆地古生产力的定量化研究比较欠缺,仅在有机碳、生物硅及生物标志化合物指标方面建立了数学模型,且多是对海相盆地古生产力指标的直接沿用;而在色素、湖相碳酸盐等具陆相特点的指标方面仅见部分定性研究。在地学应用方面,以陆相盆地古生产力研究为基础的地球生物学方法,在正演陆相烃源岩的形成过程研究中具有良好的前景。     

邻二氮杂菲银/蒙脱石复合物的XPS和TG研究

用微波辐射法制备了邻二氮杂菲银/蒙脱石抗菌复合物。以X射线光电子能谱(XPS)及热重分析(TG/DTG)对抗菌复合物及其热处理产物的表面特性及热稳定性进行探讨。结果表明:邻二氮杂菲银络离子插入到蒙脱石层间后,层间水含量减少。样品表面的银以邻二氮杂菲银络合物的状态存在,煅烧温度低于或等于200℃时,邻二氮杂菲银络合物没有发生分解;当煅烧温度到达300℃时,邻二氮杂菲银络合物开始分解产生新的物质Ag2O;当煅烧温度到达400℃时,样品表面开始有银粒子产生,随着温度的增加,银粒子的粒径不断增加。     

小秦岭地区金矿成矿机理分析

小秦岭成矿带是我国重要的贵金属成矿带之一,金矿受地层、构造和岩浆岩控制,具有＂三位一体＂的成矿模式。太古宙太华群地层为成矿提供了物质基础,区域变质作用使金发生初次富集;早期自北而南的挤压形成规模巨大的推覆构造为含金石英脉的生成提供了有利空间;燕山期构造—岩浆活动对金的活化、迁移、富集起主导作用     

硅藻提纯方法新进展:小个体硅藻纯化的实验技术

硅藻壳体氧同位素是近年来发展起来的一种重要的古气候研究手段[1～3],硅藻的分离提纯是开展此项研究的重要一环.矿物杂质由于与硅藻壳体的氧同位素差异很大[1,4,5],对目前常用的硅藻氧同位素实验方法[1,4]获得的结果有显著影响.