Determination of source parameters of small earthquakes in the east part of Guandong and south part of Fujian Province

Determination of source parameters of small earthquakes from amplitude ratios of and is studied in this paper when the distribution of the regional seismic network is skew to the earthquakes. The distribution of stations of the seismic network was to one side of the 17 earthquakes chosen from among 39 earthquakes in the east part of Guangdong and south part of Fujiang Province. The distribution of stations was classified into three types according to their relative positions with respect to the chosen earthquakes and the experiments of artificial data were done. Excellent results were also presented in various unfavourable conditions by using the method. As to the 39 small earthquakes recorded by the network in east Guangdong and south Fujian Province from 1982 to 1986, the results can be summarized as follows: Most of the fault planes of the earthquakes apear to be steep. Most of the principal compression stressesP and tensile stressesT are nearly horizontal, concentrating in the WNW-ESE direction. The Chinese version of this paper appeared in the Chinese edition ofActa Seismologica Sinia,13, 420–429, 1991.     

Seismic hazard in East Africa: An example of the application of incomplete and uncertain data

Earthquake hazard parameters maximum regional magnitude M _max and annual activity rate , and the b parameter of the Gutenberg-Richter relation have been evaluated for parts of East Africa. The applied maximum likelihood method permits the combination of both historical and instrumental data available (the catalog used here covers the interval 1880–1979). In addition, the uncertainty involved in magnitude determination and thresholds of completeness were taken into account. The hazard-parameter determination was performed for two study areas corresponding to segments of the eastern and western branches of the East African rift system. The results for these areas show differences that can be partly explained through the characteristics of the data.     

基于Hoek-Brown准则的节理岩体能量参数估算

岩体变形和破坏可以看作能量耗散和释放的过程.由于节理岩体结构复杂且难以开展室内试验,因此无法通过试验直接求取其能量学参数.基于Hoek-Brown准则和岩石能量理论,提出了节理岩体在临界状态能量学参数的估算方法.针对含贯通节理(或层面)岩体,通过修正岩块单轴抗压强度以体现贯通节理的方向效应.采用PFC3D分别模拟小尺寸岩样(Φ50mm×100mm)和大尺寸岩体(Φ2m×2m)的三轴压缩试验,通过岩石三轴试验结果拟合岩石数值模拟的细观参数并应用于节理岩体的模拟.根据节理岩体模拟得到应力应变曲线和能量流,验证了Hoek-Brown准则对节理岩体能量参数估算的合理性.     

Strong size evolution of the most massive galaxies since z∼ 2

Using the combined capabilities of the large near-infrared Palomar/DEEP-2 survey, and the superb resolution of the Advanced Camera for Surveys HST camera, we explore the size evolution of 831 very massive galaxies  ( M _⋆≥ 10¹¹ h ⁻²₇₀ M_⊙)  since   z ∼ 2  . We split our sample according to their light concentration using the Sérsic index n . At a given stellar mass, both low  ( n < 2.5)  and high  ( n > 2.5)  concentrated objects were much smaller in the past than their local massive counterparts. This evolution is particularly strong for the highly concentrated (spheroid like) objects. At   z ∼ 1.5  , massive spheroid-like objects were a factor of 4 (±0.4) smaller (i.e. almost two orders of magnitudes denser) than those we see today. These small sized, high-mass galaxies do not exist in the nearby Universe, suggesting that this population merged with other galaxies over several billion years to form the largest galaxies we see today.     

The effect of dust on Tremaine–Weinberg measurements

We investigate the effect of dust on the observed rotation rate of a stellar bar. The only direct way to measure this quantity relies on the Tremaine & Weinberg (TW) method which requires that the tracer satisfies the continuity equation. Thus, it has been applied largely to early-type barred galaxies. We show using numerical simulations of barred galaxies that dust attenuation factors typically found in these systems change the observed bar pattern speed by 20–40 per cent. We also address the effect of star formation on the TW method and find that it does not change the results significantly. The results presented here suggest that applications of the TW method can be extended to include barred galaxies covering the full range of Hubble type.