东疆红山Cu-Au矿床氧化带硫酸盐矿物穆斯堡尔谱特征及其意义

穆斯堡尔谱对确定铁离子占位、核外环境及氧化态方面有着独特的优势。在红山铜金矿床氧化带硫酸盐矿物的XRD、TA、湿法化学分析和红外光谱测试的基础上,测定了板铁矾、针绿矾等8种硫酸盐矿物的室温57Fe穆斯堡尔谱,并根据常温下硫酸盐矿物穆斯堡尔谱参数和其晶体结构中Fe3+和Fe2+的占据位置对其谱峰进行了指派。结果表明本矿床氧化带硫酸盐矿物的穆斯堡尔谱的同质异能位移较小、四级矩分裂值分布范围较大、无磁超精细分裂等特征,且硫酸盐矿物结构中存在着共价键。通过与青海锡铁山铅锌矿氧化带硫酸盐矿物的穆斯堡尔谱相比较,两者在近地表风化及氧化过程中所处的物理化学条件基本相同,酸性和氧化性的环境为硫酸盐矿物的产生和保存提供了良好条件,但红山矿床更为干旱少雨,导致两者硫酸盐的穆斯堡尔谱参数略有不同。     

茶尖岭矿区M28异常分布区银多金属矿源条件浅析

茶尖岭矿区M28异常分布区银多金属矿的形成与燕山期中酸性浅成岩浆岩有空间、成因联系,属于浅成热液矿床中的矽卡岩型成因。银多金属的成矿是热液活动、构造作用的产物,根据地层中元素的初始含量及矿源岩来阐明该异常分布区银多金属矿源条件。初步分析认为,板岩类及闪长玢岩为M28异常分布区的矿源岩,该异常分布区地层中银多金属元素的初始含量较高,该异常分布区银多金属成矿的矿源条件比较好。     

Disc precession in the M31 dipping X-ray binary Bo 158?

We present results from three XMM–Newton observations of the M31 low mass X-ray binary (LMXB) XMMU J004314.4+410726.3 (Bo 158), spaced over 3 d in 2004 July. Bo 158 was the first dipping LMXB to be discovered in M31. Periodic intensity dips were previously seen to occur on a 2.78-h period, due to absorption in material that is raised out of the plane of the accretion disc. The report of these observations stated that the dip depth was anticorrelated with source intensity. In light of the 2004 XMM–Newton observations of Bo 158, we suggest that the dip variation is due to precession of the accretion disc. This is to be expected in LMXBs with a mass ratio ≲0.3 (period ≲4 h), as the disc reaches the 3:1 resonance with the binary companion, causing elongation and precession of the disc. A smoothed particle hydrodynamics simulation of the disc in this system shows retrograde rotation of a disc warp on a period of  ∼11 P _orb  , and prograde disc precession on a period of  29 ± 1 P _orb  . This is consistent with the observed variation in the depth of the dips. We find that the dipping behaviour is most likely to be modified by the disc precession, hence we predict that the dipping behaviour repeats on an  81 ± 3 h  cycle.     

通海台垂直摆受建筑载荷影响的数值模拟研究

针对通海台垂直摆NS和EW测项自2019-04出现同步趋势转折变化,计算2017~2020年NS和EW测项M₂波潮汐因子。结合监测井等地下介质结构资料,构建通海台沿垂向分层的三维有限元物理模型,定量分析不同岩石参数模型下建筑载荷对通海台NS向及EW向位移影响的差异特征。结果表明：1）2019-04后NS测项N倾变化量达到约2 750 ms,而EW测项E倾变化量达到约580 ms,NS测项趋势变化量显著大于EW测项;2）2017~2020年NS和EW测项M₂波潮汐因子较为稳定,NS测项M₂波潮汐因子在0.7左右波动,EW测项M₂波潮汐因子在0.52左右波动,数据的转折变化未能在潮汐频段引起同步变化;3）位于通海台东北部的医院建筑物载荷在通海台附近产生N向和E向位移加载,与垂直摆NS和EW测项在2019-04后出现的N倾和E倾趋势转折变化较为一致,模拟得到的N向位移量约为E向位移量的3倍。     

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计算机图像处理在增强华县地震构造遥感信息中的应用

由于地震构造的许多重要信息在卫片上显示往往比较隐晦，必须对其进行增强处理，以取得最佳的解译效果。本文以历史上曾发生过八级地震的华县地震构造带为例，讨论辐射增强、多波段频谱变换、空间变换假彩色增强、分类等计算机图象处理方法的若干功能，以及这些功能在不同背景条件下的处理效果，为分析该地区活动断裂、地质构造等提供了有意义的信息，也为这种处理手段在地震构造信息分析等方面的推广应用提供参考。     

Global very long-baseline interferometry observations of compact radio sources in M82

Observations of the starburst galaxy, M82, have been made with a 20-station global very long-baseline interferometry (VLBI) array at λ 18 cm. Maps are presented of the brightest young supernova remnants (SNR) in M82 and the wide-field mapping techniques used in making images over a field of view of ∼1 arcmin with 3-milliarcsecond resolution are discussed. A limit has been placed on the power-law deceleration of the young supernova remnant (SNR) 43.31+592 with an index greater than 0.73±0.11 from observations with the European VLBI Network. Using the global array we have resolved compact knots of radio emission in the source which, with future global observations, will enable better constraints to be placed on the expansion parameters of this SNR.
The latest global observations have also provided high-resolution images of the most compact radio source in M82, 41.95+575. We determine an upper limit to the radial expansion rate along the major axis of 2000 km s⁻¹. However, the new images also show structure resembling that of collimated ejection which brings into question the previous explanation of the source as being a result of the confinement of a supernova by a high-density circumstellar medium.
It is apparent that we are now able to image the brightest supernova remnants in M82 with a linear scale which allows direct comparison with galactic SNR such as Cassiopeia A.