Fundamental parameters and new variables of the galactic open cluster NGC 7128     

Z. Balog  †  A. J. Delgado  ‡  A. Moitinho  G. F&#;rész  †  G. Kaszás  †  J. Vinkó  E. J. Alfaro 《Monthly notices of the Royal Astronomical Society》2001,323(4):872-886

CCD photometry in Johnson UBV and Strömgren uvby systems and medium-resolution spectroscopy of the galactic open cluster NGC 7128 are presented. Spectral types of the brightest 12 stars in the cluster field were determined based on equivalent widths of the H α and the He  i 6678-Å line. The spectroscopic observations also revealed two obvious and one probable Be-type stars showing H α emission. The analysis of the photometric diagrams gave a colour excess of E ( B − V )=1.03±0.06 mag, a distance modulus DM =13.0±0.2 mag and an age above 10 Myr. Time-resolved photometric observations obtained on one night resulted in the detection of short time-scale light variations of seven new and three already known variable stars in the cluster field.  相似文献   

Accretion stream mapping of HU Aquarii     

Sonja Vrielmann  Axel D. Schwope 《Monthly notices of the Royal Astronomical Society》2001,322(2):269-279

We present a new mapping algorithm, the Accretion Stream Mapping (ASM), which uses the full phase-coverage of a light curve to derive spatially resolved intensity distributions along the accretion stream in magnetic cataclysmic variables of AM Herculis type (polars). The surface of the accretion stream is approximated as a 12-sided (duodecadon-shaped) tube. After successfully testing this method on artificial data we applied it to emission-line light curves of H β , H γ and He  ii λ 4686 of the bright eclipsing polar HU Aqr. We find hydrogen and helium line emission bright in the threading region of the stream where the stream couples on to magnetic field lines. It is particularly interesting that the stream is bright on the irradiated side facing the white dwarf, which highlights the interplay of collisional and radiative excitation/ionization.  相似文献   

山东省区域地质构造演化探讨   总被引：13，自引：0，他引：13       下载免费PDF全文

宋明春  李洪奎 《山东国土资源》2001,17(6):12-21

山东省区域地质构造演化分为5个阶段.①陆核形成阶段形成太古宙高级区,地壳分异成稳定的花岗岩穹窿和活动的绿岩带,第一次克拉通化完成.②陆块发生形成阶段地壳向刚性发展,在华北陆核硅铝壳的基础上先后有3次张开、闭合裂谷作用,第二次克拉通化完成.这一阶段演化在鲁西地区主要表现为挤压作用,形成大量造山花岗岩;鲁东地区则以拉张作用为主,形成海槽,产生沉积.③秦昆洋形成演化阶段四堡期沿鲁东南部地壳拉张,在华北板块与扬子板块间形成秦昆洋.晋宁期秦昆洋关闭,华北板块与扬子板块对接碰撞,沿胶南造山带产生大量同碰撞花岗岩,同时产生超高压变质作用及形成丰富多彩的碰撞构造.晋宁运动最终形成统一的原始中国古陆,第三次克拉通化完成.④陆块发展阶段鲁西地区地壳频繁升降,形成广泛的海相及海陆交互相沉积;鲁东地区则以造山抬升为主,地层沉积较少.⑤滨太平洋发展阶段该阶段的主要特征是断块构造发育,形成盆岭构造格局,产生大陆边缘花岗岩,构造体系由古亚洲构造域转向滨太平洋构造域.  相似文献   

模糊划分矩阵在岩土参数概率分布中的应用   总被引：1，自引：0，他引：1  

刘明  熊彩霞  马金荣 《地球科学与环境学报》2002,24(4):38-41

讨论如何在小样本条件下用已有的过程经验与试验资料确定岩土参数概率分布,用模糊划分矩阵与BAYES方法相结合,给出由小样本试验数据确定岩土参数的概率分布。  相似文献   

An analytical expression for apsidal superhump precession and comparisons with numerical simulations and dwarf nova observations     

M.M. Montgomery 《Monthly notices of the Royal Astronomical Society》2001,325(2):761-766

We compare analytical expressions of precession rates from apsidal (positive) superhumps in close binary systems with numerical disc simulation results and observed values. In the analytical expressions, we include both the dynamical effects on the precession of the disc and effects caused by pressure forces that have been theorized to provide a retrograde effect (i.e. slowing) on the prograde disc precession. We establish new limits on density wave pitch angle to a normalized disc sound speed 60≥Ω_orb  d  tan  i / c >2.214 . Using average values for the density wave pitch angle i and speed of sound c , we find good correlation between numerical simulations and the analytical expression for the apsidal superhump period excess, which includes both the prograde and retrograde effects, for mass ratios of 0.025≤ q ≤0.33 . We also show good correlations with the four known eclipsing systems, OY Car, Z Cha, HT Cas, and WZ Sge. Our analytical expression for apsidal superhump period excess as a function of orbital period is consistent with the trend found in observed systems.  相似文献   

Erratum: Fluorescent H₂ in the reflection nebula NGC 2023 – I. Recent observations     

M. S. K. McCartney  P. W. J. L. Brand  M. G. Burton  A. Chrysostomou 《Monthly notices of the Royal Astronomical Society》2001,321(4):784-784

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Elastic solutions for stresses in a transversely isotropic half‐space subjected to three‐dimensional buried parabolic rectangular loads     

Cheng‐Der Wang  Jyh‐Jong Liao 《国际地质力学数值与分析法杂志》2002,26(14):1449-1476

In many areas of engineering practice, applied loads are not uniformly distributed but often concentrated towards the centre of a foundation. Thus, loads are more realistically depicted as distributed as linearly varying or as parabola of revolution. Solutions for stresses in a transversely isotropic half‐space caused by concave and convex parabolic loads that act on a rectangle have not been derived. This work proposes analytical solutions for stresses in a transversely isotropic half‐space, induced by three‐dimensional, buried, linearly varying/uniform/parabolic rectangular loads. Load types include an upwardly and a downwardly linearly varying load, a uniform load, a concave and a convex parabolic load, all distributed over a rectangular area. These solutions are obtained by integrating the point load solutions in a Cartesian co‐ordinate system for a transversely isotropic half‐space. The buried depth, the dimensions of the loaded area, the type and degree of material anisotropy and the loading type for transversely isotropic half‐spaces influence the proposed solutions. An illustrative example is presented to elucidate the effect of the dimensions of the loaded area, the type and degree of rock anisotropy, and the type of loading on the vertical stress in the isotropic/transversely isotropic rocks subjected to a linearly varying/uniform/parabolic rectangular load. Copyright © 2002 John Wiley & Sons, Ltd.  相似文献   

The age of the Geminids: a constraint from the spin-up time-scale     

Martin Beech 《Monthly notices of the Royal Astronomical Society》2002,336(2):559-563

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Evolution of the luminosity function and colours of galaxies in a Λ cold dark matter universe     

K. Nagamine †  M. Fukugita  R. Cen  J.P. Ostriker 《Monthly notices of the Royal Astronomical Society》2001,327(1):L10-L14

The luminosity function of galaxies is derived from a cosmological hydrodynamic simulation of a Λ cold dark matter universe with the aid of a stellar population synthesis model. At     , the resulting B -band luminosity function has a flat faint-end slope of     with the characteristic luminosity and the normalization in fair agreement with observations, while the dark matter halo mass function is steep with a slope of     . The colour distribution of galaxies also agrees well with local observations. We also discuss the evolution of the luminosity function, and the colour distribution of galaxies from     to 5. A large evolution of the characteristic mass in the stellar mass function as a result of number evolution is compensated by luminosity evolution; the characteristic luminosity increases only by 0.8 mag from     to 2, and then declines towards higher redshift, while the B -band luminosity density continues to increase from     to 5 (but only slowly at     .  相似文献   

The re-analysis of the ROSAT data of Nova Mus 1983 using white dwarf atmosphere emission models     

&#;. Balman  J. Krautter 《Monthly notices of the Royal Astronomical Society》2001,326(4):1441-1447

The analyses of X-ray emission from classical novae during the outburst stage have shown that the soft X-ray emission below 1 keV, which is thought to originate from the photosphere of the white dwarf, is inconsistent with the simple blackbody model of emission. Thus, ROSAT Position Sensitive Proportional Counter (PSPC) archival data of the classical Nova Mus 1983 (GQ Mus) have been re-analysed in order to understand the spectral development in the X-ray wavelengths during the outburst stage. The X-ray spectra are fitted with the hot white dwarf (WD) atmosphere emission models developed for the remnants of classical novae near the Eddington luminosity. The post-outburst X-ray spectra of the remnant white dwarf are examined in the context of evolution on the Hertzsprung–Russell diagram using C–O enhanced atmosphere models. The data obtained in 1991 August (during the ROSAT All Sky Survey) indicate that the effective temperature is         . The 1992 February data show that the white dwarf had reached an effective temperature in the range         with an unabsorbed X-ray flux (i.e. ∼ bolometric flux) between     and     . We show that the H burning at the surface of the WD had most likely ceased at the time of the X-ray observations. Only the 1991 August data show evidence for ongoing H burning.  相似文献