Mass segregation in young compact clusters in the Large Magellanic Cloud – III. Implications for the initial mass function     

R. de Grijs  G. F. Gilmore  A. D. Mackey  M. I. Wilkinson  S. F. Beaulieu  R. A. Johnson  B. X. Santiago 《Monthly notices of the Royal Astronomical Society》2002,337(2):597-608

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地震序列类型早期判断的可能性   总被引：2，自引：0，他引：2  

吴开统  彭克银 《地震》1996,16(1):1-8

详细讨论利用地震现场提供的１天、３天和７天观测资料，预测地震序列类型和最大强余震震级的可能性和现实性。４７个Ｍ≥６．０地震的地震序列实例检验表明，利用７天内的观测资料，准确率可达到８５．１％。因此，使用ｂ值横截距法有可能在早期预测最大强余震的震级并判断地震序列的类型。  相似文献   

Spot modelling and elements of the RS CVn eclipsing binary WY Cancri     

P. Vivekananda Rao  M. B. K. Sarma  B. V. N. S. Prakash Rao 《Journal of Astrophysics and Astronomy》1991,12(3):225-263

Results of analysis of photoelectric observations of the RS CVn eclipsing binary WY Cancri in the standard passbands ofUBV during 1973-74, 1976-79 and inUBVRI during 1984-86 are reported. A preliminary analysis of the eclipses suggested the primary eclipse to be transit. A study of the percentage contribution of the distortion wave amplitudes in all the colours with respect to the luminosities of both components, showed the hotter component to be the source of the distortion wave. The clean (wave removed) light curves of different epochs have not merged, suggesting residual effects of spot activity. The reason for this is attributed to the presence of either (1) polar spots or (2) small spots uniformly distributed all over the surface of the hotter component. This additional variation is found to have a periodicity of about 50 years or more. The distortion waves in yellow colour are modelled according to Budding’s (1977) method. For getting the best fit of the observations and theory, it was found necessary to assume three or four spots on the surface of the hot component. Out of these four spot groups, three are found to have direct motion with migration periods of 1.01, 1.01 and 2.51 years while the fourth one has a retrograde motion with a migration period of 3.01 years. From these periods and the latitudes of the spots derived from the model a co-rotating latitude of 4ℴ is obtained. The temperatures of these spots are found to be lower than that of the photosphere by about 700ℴK to 800ℴK. Assuming the light curve of 1985-86, which is the brightest of all the observed seasons, to be least affected by the spots, the light curves of the other seasons are all brought up to the quadrature level of this season by applying suitable corrections. The merged curves in theUBVRI colours are analysed for the elements by the Wilson-Devinney method. This analysis yielded the following absolute elements:

相似文献    604. CHAMP星载加速度计数据分析      王庆宾  吴晓平  王世忠 《测绘学院学报》2006,(1) 利用GFZ数据中心提供的CHAMP卫星星载加速度计数据,通过坐标系转换计算得到惯性系下的非保守力加速度;研究和讨论了CHAMP星载加速度计数据特点、改正数计算和姿态数据间断的处理等问题,指出了1.0版姿态数据跳变和2004年后姿态数据间断过大而无法使用的现象,建议实际处理时不采用1.0、1.1版及2004年后的数据。通过计算表明:在1 min之内的CHAMP星载加速度数据间断可以用简单内插的方法进行处理,并且简单内插结果的精度与数据质量有关,因此要慎重使用内插数据。  相似文献    605. 一种高精度星载导航星库的构建方法      蔡志武  韩春好  陈金平 《测绘学院学报》2006,(1) 在选用高精度基本星表的基础上,分析了导航星的选取方法及其分布特征。为了利用导航星的观测位置信息,给出了从星表平位置到星心视位置的高精度转换方法。基于分区法制定了导航星库,并给出了存储及读取方法,对该星库的访问具有简单、快速、占用资源少等优点,适合星载使用。  相似文献    606. 弹道导弹的GNSS/SST/SINS组合导航系统研究   总被引：2，自引：0，他引：2   康国华  刘建业  熊智  祝燕华 《武汉大学学报(信息科学版)》2006,31(2):176-179 提出一种组合导航方案，该方案在硬件上采用全捷联的结构，在算法上将捷联星光跟踪仪（strapdown startracker，SST）的姿态信息，高动态GNSS的位置、速度信息与捷联惯导进行组合滤波，全面提高导航精度。设计并实现了弹道导弹GNSS／SST／SINS组合导航系统实时仿真平台，仿真结果表明了该组合方案的稳定、可靠性。  相似文献    607. Two serendipitous low-mass LMC clusters discovered with HST1      Basílio X. Santiago  Rebecca A. W. Elson  Steinn Sigurdsson  & Gerard F. Gilmore 《Monthly notices of the Royal Astronomical Society》1998,295(4):860-868 We present V and I photometry of two open clusters in the LMC down to V ∼26. The clusters were imaged with the Wide Field and Planetary Camera 2 (WFPC2) on board the Hubble Space Telescope ( HST ), as part of the Medium Deep Survey Key Project. Both are low-luminosity ( MV ∼−3.5), low-mass ( M ∼103 M⊙) systems. The chance discovery of these two clusters in two parallel WFPC2 fields suggests a significant incompleteness in the LMC cluster census near the bar. One of the clusters is roughly elliptical and compact, with a steep light profile, a central surface brightness μ V (0)∼20.2 mag arcsec−2, a half-light radius r hl∼0.9 pc (total visual major diameter D ∼3 pc) and an estimated mass M ∼1500 M⊙. From the colour–magnitude diagram and isochrone fits we estimate its age as τ∼(2–5)×108 yr. Its mass function has a fitted slope of Γ=Δlogφ( M )/Δlog M =−1.8±0.7 in the range probed (0.9≲ M /M⊙≲4.5). The other cluster is more irregular and sparse, having shallower density and surface brightness profiles. We obtain Γ=−1.2±0.4, and estimate its mass as M ∼400 M⊙. A derived upper limit for its age is τ≲5×108 yr. Both clusters have mass functions with slopes similar to that of R136, a massive LMC cluster, for which HST results indicate Γ∼−1.2. They also seem to be relaxed in their cores and well contained in their tidal radii.  相似文献    608. Evolutionary synthesis of stellar populations: a modular tool   总被引：1，自引：0，他引：1   Claudia Maraston 《Monthly notices of the Royal Astronomical Society》1998,300(3):872-892 A new tool for the evolutionary synthesis of stellar populations is presented, which is based on three independent matrices, giving respectively (1) the fuel consumption during each evolutionary phase as a function of stellar mass, (2) the typical temperatures and gravities during such phases, and (3) the colours and bolometric corrections as functions of gravity and temperature. The modular structure of the code allows one easily to assess the impact on the synthetic spectral energy distribution of the various assumptions and model ingredients, such as, for example, uncertainties in stellar evolutionary models, the mixing length, the temperature distribution of horizontal branch stars, asymptotic giant branch mass loss, and colour–temperature transformations. The so-called 'AGB phase transition' in Magellanic Cloud clusters is used to calibrate the contribution of the thermally pulsing asymptotic giant branch phase to the synthetic integrated luminosity. As an illustrative example, solar-metallicity ( Y  = 0.27, Z  = 0.02) models, with ages ranging between 30 Myr and 15 Gyr and various choices for the slope of the initial mass function, are presented. Synthetic broad-band colours and the luminosity contributions of the various evolutionary stages are compared with Large Magellanic Cloud and Galactic globular cluster data. In all these cases, a good agreement is found. Finally, the evolution is presented of stellar mass-to-light ratios in the bolometric and U B V R K passbands, in which the contribution of stellar remnants is accounted for.  相似文献    609. The dynamical evolution of stellar superclusters      Pavel Kroupa 《Monthly notices of the Royal Astronomical Society》1998,300(1):200-204 Recent images taken with the Hubble Space Telescope ( HST ) of the interacting disc galaxies NGC 4038/4039 (the Antennae) reveal clusters of many dozens and possibly hundreds of young compact massive star clusters within projected regions spanning about 100 to 500 pc. It is shown here that a large fraction of the individual star clusters merge within a few tens to a hundred Myr. Bound stellar systems with radii of a few hundred parsecs, masses ≲ 109 M⊙ and relaxation times of 1011 − 1012 yr may form from these. These spheroidal dwarf galaxies contain old stars from the pre-merger galaxy and much younger stars formed in the massive star clusters, and possibly from later gas accretion events. The possibility that star formation in the outer regions of gas-rich tidal tails may also lead to superclusters is raised. The mass-to-light ratio of these objects is small, because they contain an insignificant amount of dark matter. After many hundred Myr such systems may resemble dwarf spheroidal satellite galaxies with large apparent mass-to-light ratios, if tidal shaping is important.  相似文献    610. Infrared observation and the energy distribution of silicate carbon stars      Pei-sheng Chen  Guan-zhu Xiong  Xun-hao Wang 《Chinese Astronomy and Astrophysics》1998,22(4):147-478 Near-infrared photometry of all 11 silicate carbon stars north of declination −10° is made. Combined with available data in the visible range and from IRAS, we discuss their distribution on the infrared two-color diagrams and their spectral distribution, and we compare with the results for normal carbons and so ascertain their evolutionary status.  相似文献    [首页] « 上一页 [56] [57] [58] [59] [60] 61 [62] [63] [64] [65] [66] 下一页 » 末  页»