On the mass of M31

Recent work by several groups has established the properties of the dwarf satellites to M31. We reexamine the reported kinematics of this group employing a fresh technique we have developed previously. By calculating the distribution of a χ statistic (which we define in the paper) for the M31 system, we conclude that the total mass (disc plus halo) of the primary is unlikely to be as great as that of our own Milky Way. In fact the χ distribution for M31 indicates that, like NGC 3992, it does not have a massive halo. In contrast, the analysis of the satellites of NGC 1961 and NGC 5084 provides strong evidence for massive haloes surrounding both spiral galaxies.     

Narrow-band CCD photometry of giant H ii regions

We have obtained accurate CCD narrow-band Hβ and Hα photometry of giant H  ii regions (GEHRs) in M33, NGC 6822 and M101. Comparison with previous determinations of emission-line fluxes shows large discrepancies; their probable origins are discussed. Combining our new photometric data with global velocity dispersion ( σ ) derived from emission linewidths, we review the     relation. A re-analysis of the properties of the GEHRs included in our sample shows that age spread and the superposition of components in multiple regions introduce a considerable spread in the regression. Combining the information available in the literature regarding ages of the associated clusters, evolutionary footprints on the interstellar medium, and kinematical properties of the knots that build up the multiple GEHRs, we find that a subsample – which we refer to as young and single GEHRs – do follow a tight relation in the     plane.     

Characterization of a chalcopyrite from Brazil by Mössbauer spectroscopy and other physicochemical techniques

We studied a chalcopyrite from a Cu ore deposit in Rio Grande do Sul, Brazil, by Mössbauer spectroscopy at room temperature and 110 K. Supporting methods to check for sample purity and to characterize further sample properties were slow-scanning X-ray powder diffraction and optical and microprobe analyses of polished sections of selected grains. Chemical analyses obtained using a scanning electron microscope equipped with an energy-dispersive X-ray spectrometer showed the sample to consist of homogeneous and essentially stoichiometric chalcopyrite (CuFeS₂). Mössbauer spectra taken at both the above temperatures consist of asymmetric magnetically ordered patterns with unequal intensities of the line pairs 1–6 and 2–5, pointing to the existence of non-equivalent or multiple Fe sites. Least-squares fittings evidenced that the resonance intensity ratio of subspectrum with lower quadrupole shift (indicative of a more symmetric environment) to that with higher shift is 69:31, at room temperature, and 68:32, at 110 K. Rietveld refinement of the XRD data indicates the existence of tetragonal [a = 0.52855(1) and c = 1.0412(1) nm] and cubic [a ₀ = 0.5273(2) nm] modifications in a proportion of 74:26, in good agreement with the Mössbauer data. The saturation magnetization of the sample was 32.7 J/(T kg), confirming the oxidation state of Fe as trivalent and pointing to little to no spin canting.     

自动推算室内接入点坐标算法

随着基于位置服务的应用与发展,室外和室内定位技术都得到了飞速发展。特别是在WiFi定位技术的不断完善下,室内定位技术有了广泛的应用,但是,WiFi定位技术的两种定位方式均需预先知道室内网络接入点的精确坐标,这一要求无法满足一些紧急情况下的定位需求。因此,本文提出了一种基于M估计的自动推算室内接入点坐标算法。该算法借助在室内外交界处同时获取卫星定位信息和WiFi信号的RSSI信息,巧用分段RSSI测距算法提高长距离RSSI测距精度,结合残差绝对和最小的M估计改进距离交会定位算法,最终推算出室内接入点的三维坐标,实现自动化推算过程。试验结果表明：该方法的定位精度比常规距离交会最小二乘算法提高了50%,能够快速实时较精确地推算室内接入点的坐标,进一步完善了WiFi定位技术。     

2014年康定M_S6.3级地震前后的重力变化特征

利用四川地区2010年8月至2015年3月的流动重力观测数据作出重力场等值线变化图像,研究分析2014年康定MS6.3级地震前后的重力变化特征,结果表明:(1)三岔口地区长期保持区域性重力正值变化异常及重力变化高梯度带;(2)在康定MS6.3级地震前后三岔口地区的区域性重力正值变化异常及重力变化高梯度带变化并不是特别显著;(3)在康定MS6.3级地震前震区重力变化等值线出现四象限区域或者类似于四象限区域的分布特征;(4)康定MS6.3级地震发震位置处于0值线附近且0值线在此处发生明显的转折、畸变;(5)康定MS6.3级地震发生在重力减小后回调增加的过程中,震后重力继续回调增加。     

Hydro-meteorological drought assessment under climate change impact over the Vu Gia–Thu Bon river basin,Vietnam

Hydro-meteorological drought was assessed with respect to climate change over an estuary catchment Vu Gia-Thu Bon in Central Vietnam, which economy is dependent on agriculture. The fully-distributed hydrological model MIKE SHE was used to simulate river flow over the study region for the period 1991–2010. Drought were assessed using the Standardized Precipitation Index and the Standardized Runoff Index. The future climate was studied using the regional climate model Weather Research and Forecasting by downscaling an ensemble of three global climate models – CCSM3.0, ECHAM5 and MIROC-medium resolution over current (1961–1990) and future climates (2011–2040), under the A2 emissions scenario. The results suggest that, despite hotter and wetter future climate, the area is likely to suffer more from severe and extreme droughts, increasing about 100% in the median range for drought characteristics. Thus, there is a need for proper adaptation and planning for water resources management in this region.     

Is the Variable X—ray Source in M82 due to Gravitational Lensing？

1 INTRODUCTIONObservations of the most famous starburst galaxy M82 with the High-Resolution Cameraon board the Chandra X-Ray Observatory, showed that there are nine sources in the celltral11 x 11 region, but no son-roe was detected at the galactic center (Matsumoto et al. 2001).Comparing the observations on 1999 October 28 and those on 2000 January 20, the authorsfound an extremely large time variability of the source CXO M82 J095550.2 694047, which islocated gll away from the galact…     

汶川大地震四川省青川县砖混结构村镇房屋震害分析

2008年汶川 8.0级大地震造成了大量的房屋破坏,尤其村镇房屋的破坏最为严重.本文基于对四川省青川县部分乡镇村镇房屋震害的实地调查,对砖混结构房屋的震害从地形、地基基础和结构三方面进行了震害总结,分析了典型震害的成因,指出了目前村镇房屋建设存在的问题,最后对提高村镇民房的地震安全提出了一些建议.     

Masses of the local group and of the M81 group estimated from distortions in the local velocity field

Based on high precision measurements of the distances to nearby galaxies with the Hubble telescope, we have determined the radii of the zero velocity spheres for the local group, R₀ = 0.96±0.03Mpc, and for the group of galaxies around M 81/M 82, 0.89±0.05Mpc. These yield estimates of M_T = (1.29±0.14)· 10¹² M_⊙ and (1.03±0.17)· 10¹² M_⊙, respectively, for the total masses of these groups. The R₀ method allows us to determine the mass ratios for the two brightest members in both groups, as well. By varying the position of the center of mass between the two principal members of a group to obtain minimal scatter in the galaxies on a Hubble diagram, we find mass ratios of 0.8:1.0 for our galaxy and Andromeda and 0.54:1.00 for the M82 and M81 galaxies, in good agreement with the observed ratios of the luminosities of these galaxies. __________ Translated from Astrofizika, Vol. 49, No. 1, pp. 5–22 (February 2006).