Giant pulses from the millisecond pulsar PSR B1937+214

We have detected giant pulses from the millisecond pulsar PSR B1937+214 at the lowest frequency of 112 MHz. The observed flux density at the pulse peak is ～40 000 Jy, which exceeds the average level by a factor of 600. Pulses of such intensity occur about once per 300 000 periods. The brightness temperature of the observed giant pulses is T _B≈10³⁵ K. We estimated the pulse broadening by interstellar scattering to be τ_sc=3–10 ms. Based on this estimate and on published high-frequency measurements of this parameter, we determined the frequency dependence of the pulse broadening by scattering: τ_sc(f)=25 × (f/100)^?4.0±02.     

两类埃达克岩的含矿性和成因:东南亚地区与东太平洋带对比

新生代埃达克岩是一种新型的火成岩(Sr/Y≥20),多产出于大洋岛弧、大陆边缘造山带(东南亚地区)和陆缘火山弧环境(东太平洋带),依据REE配分模式可将其划分为2种成因类型:大洋型(O型)和大陆型(C型)。埃达克岩分别广泛分布于东南亚地区的菲律宾群岛、苏拉威西、中加里曼丹、印度尼西亚几内亚岛、巴布亚新几内亚至所罗门群岛一带,及东太平洋带的北美洲、墨西哥、中美洲、南美洲的北部至南部。研究表明:不同成因类型的埃达克岩具有不同的含矿性,反映各自岩浆源区不同。C型埃达克岩(La/Yb12)是俯冲海洋板块部分熔融叠加增厚的地壳底部部分熔融MASH(熔融-混染-储存-均一化)和AFC(混染-分异-结晶)作用的产物,多半与世界级斑岩铜金矿床共生;O型埃达克岩(La/Yb≤12)则与平缓俯冲的海洋板片部分熔融作用有关,在东南亚地区主要与浅成热泉金矿有成因联系。     

Decline of Terebralia palustris in South African mangroves

Terebralia palustris (Linnaeus, 1767), the giant mangrove whelk, is a prominent component of mangrove ecosystem malacofauna in the Indo-West-Pacific region. On the east coast of Africa, the range of T. palustris extends from Kenya to the south-eastern region of South Africa. Here we confirm reports that, in the past three decades, South African populations of T. palustris have declined. Terebralia palustris was recorded from only two estuarine mangrove forests during a survey conducted in 2013/2014, compared with six estuaries in the mid-20th century. At Kosi Bay, the average density was 186 ind. m^-2 (SD 106) in comparison to only 7.1 ind. m^-2 (SD 2.5) at Durban Bay. Additionally, the average shell height of individuals at Durban Bay (60.3 mm; SD 13.6) was larger than at Kosi Bay (31.84 mm; SD 16.09), indicating the absence of juvenile snails at Durban. In South Africa there have been no previous ecological assessments for T. palustris and, aside from one detailed survey in the early 1960s, most of the occurrence records are vague and incomplete. The ultimate causes for the decline of this charismatic gastropod in South Africa are unknown, although habitat loss and degradation are suspected. Further research is urgently required, particularly into aspects concerning its disappearance at the limit of its global distribution.     

松辽冰盖与松辽分水岭翘板迁移间的动力关系探讨

广布于松辽平原科尔沁沙地的巨型弧形沙垄的成因一直未能得到很好解释,该项研究采用罗根冰碛变形机理对该区的巨型弧形沙垄、密布的湖泡等特征地貌进行分析,发现其与斯堪的纳维亚冰盖、劳伦泰德冰盖的冰下软基变形地貌特征具有同一性,从而确认巨型弧形沙垄为冰盖冰流形成的巨型流线、罗根冰碛与锅穴构造的遗留,从而佐证了“松辽冰盖”的存在。研究发现松辽平原的巨型弧形流线显示出具有从盆地周围向沉降中心延伸、汇聚的特征,这表明流线的走向受制于地势的控制,而非所谓的风力所为。此外根据巨型冰川流线的展布形态与松辽分水岭之间存在的反常关系,发现在冰盖消融后松辽分水岭发生了北移现象,这一现象的产生可能与冰盖消融后导致的松辽盆地的失压反弹隆升有关。根据松辽分水岭的迁移时间、风沙层序年龄、荷载构造扰动地层年龄的综合约束,初步判断松辽冰盖的最近一次的发生时间在晚更新世早期(MIS4阶段)的东山冰期。     

浅议元素离子电位和丰度与巨型矿床的关系

元素的质和量及其排列组合方式被认为是矿床形成的"基因".使用离子电位与克拉克值定量反映元素的质、量特征.成矿不外乎"源、运、储"三个环节,而离子电位通过控制金属"运"的行为影响其成矿能力,笔者给出了唯一的具有一定成因意义的元素离子电位,并发现离子电位与全球巨型矿床数目(n)、吨位堆积指数(TAI)可以拟合为一条向上开口的抛物线.克拉克值通过影响元素参与成岩-成矿过程的浓度继而支配着它们的地球化学行为,笔者证实了金属累积堆积量(m)与其丰度(c)呈线性相关,暗示某元素的高丰度可能意味着该元素的区域资源优势.     

复杂巨型滑坡形成机制三维离散元模拟分析

滑坡位于金沙江下游某拟建的大型水电站库区左岸,距坝址较近,总体积约为2 560万m3,属特大型滑坡,其稳定与否将直接威胁到大坝安全和水库正常运营。由于滑坡成因复杂,对其进行合理评价和科学预测尚有困难。为此,结合野外详细勘查资料的分析,对其形成机制进行了定性分析,认为主要以滑移-弯曲型为主,局部可能存在滑移-拉裂或蠕滑-拉裂变形。在此基础上,运用三维离散元数值模拟分析方法,再现了其变形破坏演化过程,进一步证实了其滑移-弯曲型变形破坏机制,很好地解释了主滑带低于现今河床、主滑体南侧边界比较模糊等原因,从而为其发展演化趋势、稳定性和危害性评价提供了有力依据。     

Internal motions of HII regions and giant HII regions

We report new echelle observations of the kinematics of 30 HII regions in the LMC, including the 30 Doradus giant HII region. All of the HII regions possess supersonic velocity dispersions, which can be attributed to a combination of turbulent motions and discrete velocity splitting produced by stellar winds and/or embedded supernova remnants (SNRs). The core of 30 Dor is unique, with a complex velocity structure that parallels its chaotic optical morphology. We use our calibrated echelle data to measure the physical properties and energetic requirements of these velocity structures. The most spectacular structures in 30 Dor are several fast expanding shells, which appear to be produced at least partially by SNRs.     

Accessing High Pressure States Relevant to Core Conditions in the Giant Planets

We have designed an experimental technique to use on the National Ignition Facility (NIF) laser to achieve very high pressure (P _max > 10 Mbar = 1000 GPa), dense states of matter at moderate temperatures (T < 0.5 eV = 6000 K), relevant to the core conditions of the giant planets. A discussion of the conditions in the interiors of the giant planets is given, and an experimental design that can approach those conditions is described.     

The fundamental role of giant comets in earth history

We discuss some fundamental aspects of Earth history as predicted by what has come to be called coherent rather than stochastic catastrophism. The latter essentially seeks to provide an understanding of terrestrial evolution in terms of occasional kilometre-plus impactors from the asteroid belt whereas the former recognises a far more complex extraterrestrial regime arising from the streams of sub-kilometre and kilometre-plus debris due to the disintegration of successive giant comets in sub-Jovian orbits. Periodicities of 15 Myr during the later Phanerozoic (i.e. 250 to 0 Myr BP) and 200 yr during the Holocene (i.e. 10,000 to 0 yr 1313) are likely fundamental signatures in the terrestrial record relating to the action of past and present giant cornets respectively.     

Detection of giant pulses from the pulsar PSR B0031-07

Giant pulses have been detected from the pulsar PSR B0031-07. A pulse with an intensity higher than that of the average pulse by a factor of 50 or more is encountered approximately once per 300 observed periods. The peak flux density of the strongest pulse was 530 Jy, which is a factor of 120 higher than the peak flux density of the average pulse. The giant pulses are a factor of 20 narrower than the integrated profile and are clustered about its center.