海高斯”登陆海南西藏遭遇强降雪——2008年10月——

10月,全国平均气温较常年同期偏高1.1℃,平均月降水量较常年同期偏多6.4mm;上旬,0817号台风海高斯先后登陆海南和广东,部分省出现暴雨灾害;上中旬,东北、江南、西南及内蒙古等地的部分地区气象干旱发展;下旬,全国遭遇大范围降温,其中西藏遭遇强降雪天气;此外我国东部和南部的部分地区出现大雾天气.     

我国大陆上空可降水量的时空变化特征

利用1958-2001年NCEP/NCAR和ECMWF月平均再分析资料,由地面积分到300 hPa计算了我国大陆上空整层大气的可降水量,对可降水量的时空变化规律及我国大陆上空可降水总量变化特征进行了分析,并利用部分站点探空资料对大气再分析资料获得的结果进行了校验.结果表明:我国大部分地区年平均可降水量表现为减少趋势,而西北地区和华南沿海呈增加趋势;各个季节平均可降水量趋势变化特征并不相同;去除线性趋势的可降水量异常变化主要表现为全国大部分地区一致的年代际振荡,在1965年可降水量由偏多向偏少转变,而在1987年前后可降水量又由偏少向偏多转变;我国大陆上空年平均可降水总量的变化特征主要表现为从1960s中期的持续减少和大致从1980s后期的增加趋势特征.     

Attribution analyses of potential evapotranspiration changes in China since the 1960s

This paper focuses on the primary causes of changes in potential evapotranspiration (ET_o) in order to comprehensively understand climate change and its impact on hydrological cycle. Based on modified Penman-Monteith model, ET_o is simulated, and its changes are attributed by analyzing the sensitivity of ET_o to influence meteorological variables together with their changes for 595 meteorological stations across China during the period 1961–2008. Results show the decreasing trends of ET_o in the whole country and in most climate regions except the cold temperate humid region in Northeast China. For China as a whole, the decreasing trend of ET_o is primarily attributed to wind speed due to its significant decreasing trend and high sensitivity. Relative humidity is the highest sensitive variable; however, it has negligible effect on ET_o for its insignificant trend. The positive contribution of temperature rising to ET_o is offset by the effect of wind speed and sunshine duration. In addition, primary causes to ET_o changes are varied for differing climate regions. ET_o changes are attributed to decreased wind speed in most climate regions mainly distributed in West China and North China, to declined sunshine duration in subtropical and tropical humid regions in South China, and to increased maximum temperature in the cold temperate humid region.     

河南省黄淮气旋暴雨的天气特征及个例诊断

通过对1990-2001年6-8月影响河南省的18个黄淮气旋暴雨个例进行统计得知:影响河南省的黄淮气旋暴雨6月最多,7月次之,8月最少。黄淮气旋暴雨产生有两个源地,一个在河南省三花间略偏南一带,另一个在河南省南部和湖北的交界处,气旋的形成与两地向东开口的喇叭口地形有关。黄淮气旋暴雨发生前24-12 h,地面图上影响系统可分为西路冷空气影响型和倒槽顶部发展型两种;高空图上,河南多受高压脊控制,700 hPa影响系统有"人"字型切变和低槽型两种,但与地面影响系统没有直接对应关系。为了进一步揭示黄淮气旋暴雨的发生机理,利用NCEP再分析资料,对2007年7月12-15日黄淮气旋引发的暴雨天气过程进行了诊断分析,结果表明:黄淮气旋暴雨的发生、发展是大气斜压性强烈发展的结果,500 hPa高空急流和700 hPa低涡的移动方向对地面气旋的移动有引导作用。     

河南大风灾害分布特征及成因分析

本文利用全省1961-2006年的大风天气资料和大风灾情资料,对大风灾情发生的地理分布特征,月、季、年的时间变化特征进行统计分析,并对其成因作了进一步研究,结果发现,自20世纪80年代开始,大风灾情日数年际变化大幅度增加,大风日数与大风灾情日数的地理分布基本一致,大风灾情日数季节变化明显.     

The Origin of the Element Eu in Extremely Metal-poor Halo Stars

The fast neutron capture process (the r-process) occurs in the neutron-rich circumstance. However its concrete physical environment is not very clear. With recent progress in observations, many extremely metal-poor halo stars have been discovered. They have two characteristics: one is the overabundance of fast neutron elements with the relative abundance consistent with that of the sun; the other is that fast neutron element contents in stars at the same metal abundance have a very large dispersion. This provides a particular way to study the origin of the r-process. Simulation was used to study the galaxy's evolution process and the resulting dispersion of fast neutron nuclide contents in stars. The model of galaxy evolution obtained in this way not only contains spontaneous star formation in the gas region, but also includes the star formation excited by the supernova explosion. It is shown from our results that the supernovae at the low mass end should be the place producing the fast neutron nuclides. In addition, it is also shown that the non-uniformity of the galaxy evolution caused by the supernova explosion is not enough to explain the observed dispersion of fast neutron element contents in halo stars. This problem should be further studied.     

The origin of refractory minerals in comet 81P/Wild 2

Refractory Ti-bearing minerals in the calcium-, aluminum-rich inclusion (CAI) Inti, recovered from the comet 81P/Wild 2 sample, were examined using analytical (scanning) transmission electron microscopy (STEM) methods including imaging, nanodiffraction, energy-dispersive spectroscopy (EDX) and electron energy loss spectroscopy (EELS). Inti fassaite (Ca(Mg,Ti,Al)(Si,Al)₂O₆) was found to have a Ti³⁺/Ti⁴⁺ ratio of 2.0 ± 0.2, consistent with fassaite in other solar system CAIs. The oxygen fugacity (logf_O2) of formation estimated from this ratio, assuming equilibration among phases at 1509 K, is −19.4 ± 1.3. This value is near the canonical solar nebula value (−18.1 ± 0.3) and in close agreement with that reported for fassaite-bearing Allende CAIs (−19.8 ± 0.9) by other researchers using the same assumptions. Nanocrystals of osbornite (Ti(V)N), 2–40 nm in diameter, are embedded as inclusions within gehlenite, spinel and diopside in Inti. Vanadium is heterogeneously distributed within some osbornite crystals. Compositions range from pure TiN to Ti_0.36V_0.64N. The possible presence of oxide and carbide in solid solution with the osbornite was evaluated. The osbornite may contain O, but C is not present at detectable levels. The presence of osbornite, likely a refractory early condensate, together with the other refractory minerals in Inti, indicates that the parent comet contains solids that condensed closer to the proto-sun than the distance at which the parent comet itself accreted. The estimated oxygen fugacity and the reported isotopic and chemical compositions are consistent with Inti originating in the inner solar system like other meteoritic CAIs. These results provide insight for evaluating the validity of models of radial mass transport dynamics in the early solar system. The oxidation environments inferred for the Inti mineral assemblage are inconsistent with an X-wind formation scenario. In contrast, radial mixing models that allow accretion of components from different heliocentric distances can satisfy the observations from the cometary CAI Inti.     

Assessment of global meteorological,hydrological and agricultural drought under future warming based on CMIP6

在全球变暖背景下,分析和预测干旱的变化趋势和传播规律对于区域生态环境安全和灾害管理具有重要意义.本文基于第六次国际耦合模式比较计划(CMIP6),分析了SSP2-4.5和SSP5-8.5两种变暖情景下的气象(标准化降水指数SPI和标准化降水蒸发指数SPED,水文(标准化径流指数SRI)和农业(标准化土壤水分指数SSI)...     

Spinifex-like textured metaperidotites from the Higo Metamorphic Rocks,Japan, a possible high-pressure dehydration product of antigorite serpentinite

Spinifex-like textured metaperidotites from the Higo Metamorphic Rocks (HMR), west-central Kyushu, Japan, may be formed by high-pressure dehydration of antigorite, and may indicate deep subduction of serpentinite reaching a pressure–temperature condition of 1.6 GPa and 740–750 °C. Three rock types have been identified based on mineral assemblage and rock texture: Type I (L) consisting of medium-grained (1–5 cm long) olivine + enstatite + chromite ±tremolite with secondary talc and anthophyllite that occurs in low-grade metamorphic rocks of the biotite zone, Type I (H) of coarse-grained (up to 10 cm long) olivine + enstatite (with clinoenstatite lamella) + chromite ±tremolite with secondary talc that occurs in high-grade metamorphic rocks of the garnet-cordierite zone, and Type II composed of Al-spinel + chlorite + olivine + apatite + ilmenite with minor sodic gedrite in the garnet-cordierite zone together with Type I (H). Olivines in all rock types are mostly serpentinized during exhumation. The chromite-olivine thermometer gives 560–690 °C for Type I (L) rocks, and the spinel-olivine thermometer gives 610–740 °C for Type II rocks. The peak metamorphic pressure will be higher than 1.6 GPa based on the location of the experimentally determined invariant point (P = 1.6 GPa and T = 670 °C) of antigorite + forsterite + enstatite + talc + H₂O. This estimate is consistent with the occurrence of chlorite in Type II rocks, which is stable up to 890 °C at 2.0 GPa. The spinifex-like textured metaperidotites occur as small bodies in the low P/T type gneisses, implying tectonic juxtaposition of them probably during exhumation of the HMR. Recent findings of medium pressure (0.9–1.2 GPa) granulites and gneisses from the HMR may indicate that the HMR has a deep root into the wedge mantle from which the spinifex-like textured metaperidotites have derived.     

The Structure of Narrow-Line Region in LINERs

Low-ionization nuclear emission regions (LINERs) are present in a large fraction of local galaxies, while their connection to the more luminous active galactic nuclei (AGN) remains elusive. We analyze the narrow band images obtained by the Hubble Space Telescope (HST) in Hα [NⅡ] and/or [OⅢ] band for 23 LINERs and low luminosity Seyfert galaxies in the sample of the Palomar Optical Spectroscopic Survey of nearby galaxies in an attempt to resolve the structure of Narrow Emission Line Regions (NLRs) of these objects. In all cases, NLRs are well resolved and their morphology differs from object to object. Clumps, linear structure, spiral arms or a ring are detected in a large fraction of the objects, while there is no significant difference between Seyfert galaxies and LINERs. We find that the NLR size and the narrow line luminosity are strongly correlated for both LINERs and low luminosity Seyfert galaxies, and that the size of Hα [NⅡ] emission line region scales with Hα luminosity as RNLR∞L0.4±0.06Hα, consistent with an extension of the NLR size-luminosity relation defined for luminous Seyfert galaxies and quasars, to two orders of magnitude lower in luminosity and to lower activity levels. Our results suggest that NLRs in LINERs are similar to those of Seyfert galaxies, and they are powered by the central active galactic nucleus.