断层破裂速度对地震动及其地震灾害影响的有限单元法模拟

断层破裂传播速度通常会影响强地面运动加速度的空间分布及地震的灾害程度,但究竟是如何影响的,目前未见全面的定量分析.为此,本研究设断层破裂速度从小到大发生改变(从亚剪切波速度到超剪切破裂速度),同时利用有限元方法计算在不同破裂传播速度的情况下,破裂产生的地震动及强地面运动峰值加速度(PGA)的空间分布,计算时保持在所有情况下其断层上的最终位错相等,即所有不同破裂情况下产生的地震矩震级保持不变,都为MW=7.0.计算结果显示：总体上,破裂传播的速度越快,PGA的幅值越大并且高值区分布的范围也越广,其地震灾害会越严重;超剪切破裂相对于亚剪切破裂会加剧地震灾害.但是,当破裂速度正好等于介质的剪切波速度时,断层面附近PGA峰值最大,断层附近的地震灾害最为严重.此外,研究中还发现,当破裂传播速度等于倍剪切波速度时(该速度称为Eshelby速度),不产生剪切马赫波;这与超剪切破裂产生剪切马赫波的普遍现象不一致;但此时PGA并没有大幅度减小,其震害也不会有显著改变.因此,本研究对于深入认识地震震源过程、地震动效应以及灾害评估有着重要的科学意义及实用价值.     

蛇纹石化方辉橄榄岩弹性波速实验研究及其在地幔楔中的应用

地幔楔是俯冲带系统的重要组成单元, 在地球内部物质循环、壳幔相互作用过程中起着承上启下的关键作用。俯冲板片脱水可以引起上覆地幔楔中橄榄岩类的蛇纹石化, 而蛇纹石的波速显著低于地幔橄榄岩, 所以不同蛇纹石化程度的地幔楔表现出不同的低速特征。本研究首先利用天然叶蛇纹石热压合成纯的蛇纹岩样品, 利用橄榄石和斜方辉石热压合成方辉橄榄岩样品, 然后在高压下分别测量合成的方辉橄榄岩和蛇纹岩样品的纵波速度(V_P)和横波速度(V_S), 结合Voigt-Reuss-Hill岩石物理模型计算得到不同蛇纹石含量的方辉橄榄岩的波速, 最后结合地震波资料, 估算出不同俯冲带地幔楔的蛇纹石化程度。研究表明, 在地幔楔蛇纹石化程度和含水量的估算中, 必须考虑斜方辉石蛇纹石化的影响。相比前人研究, 方辉橄榄岩的蛇纹石化可能更接近于实际情况。

     

Photometric membership and metallicities of red giant candidates in selected open clusters

As part of a long‐term project to determine abundances and astrophysical properties of evolved red stars in open clusters, we present high‐precision DDO photoelectric observations for a sample of 33 red giant candidates projected in the fields of nine Galactic open clusters. These data are supplemented with UBV photoelectric photometry of 24 of these stars as well as with CORAVEL radial‐velocity observations for 13 red giant candidates in four of the clusters. We also present Washington photoelectric photometry of a small sample of red giant candidates of the open cluster Ruprecht 97. The likelihood of cluster membership for each star photometrically observed and for 23 additional red giant candidates with UBV and DDO data available in the literature, is evaluated by using two independent photometric criteria. Nearly 82% of the analysed stars are found to have a high probability of being cluster giants. Photometric membership probabilities show very good agreement with those obtained from CORAVEL radial velocities. While E (B –V) colour excesses were determined from combined B – V and DDO colours, calibrations of the DDO system were used to derive MK spectral types, effective temperatures and metallicities. The derived DDO metallicities range between values typical of moderately metal‐poor clusters ([Fe/H] = –0.19) to moderately metal‐rich ([Fe/H] = 0.25) ones. (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Spectroscopic verification of suspected planetary nebulae. IV.

Verification of 7 objects as PNe (Table 1/A) as well as misclassification of 5 objects as PNe (Table 1/C) are discussed according to our CCD spectra; the status of 4 objects (Table 1/B) remains uncertain. In Table we give the estimates of line‐strengths and the measured intensities of emission lines as well as the derived hel. radial velocities and their standard deviations.     

Kinematics of 11 Bidelman's weak‐lined stars

Radial velocities obtained with the CORAVEL‐type spectrometer are presented for 11 Bidelman's weak‐lined stars, classified from moderate dispersion objective prism spectra. Standard errors of the measurements are smaller than 1 km/s. For five of these stars, measured in the Vilnius photometric system, only small metal deficiency is established. Kinematically, most of the stars belong to the thin disk and only two stars, HD 71185 and BD +75° 641, are consistent with membership of the thick disk population.     

Spectroscopic verification of suspected planetary nebulae. III.

Classification of eight objects as planetary nebulae (Table I/A) was confirmed according to our image tube spectra; as to further two objects (Table 1/B) their status remains unclear. In Table 2 we give estimates of line-strengths, derived heliocentric radial velocities and their standard deviations.