A 'super' star cluster grown old: the most massive star cluster in the Local Group

We independently redetermine the reddening and age of the globular cluster (GC) 037−B327 in M31 by comparing independently obtained multicolour photometry with theoretical stellar population synthesis models. 037−B327 has long been known to have a very large reddening value, which we confirm to be   E ( B − V ) = 1.360 ± 0.013  , in good agreement with the previous results. We redetermine its most likely age at  12.4 ± 3.2 Gyr  .
037−B327 is a prime example of an unusually bright early counterpart to the ubiquitous 'super' star clusters presently observed in most high-intensity star-forming regions in the local Universe. In order to have survived for a Hubble time, we conclude that its stellar initial mass function (IMF) cannot have been top-heavy. Using this constraint, and a variety of simple stellar population (SSP) models, we determine a photometric mass of     , somewhat depending on the SSP models used, the metallicity and age adopted and the IMF representation. This mass, and its relatively small uncertainties, makes this object the most massive star cluster of any age in the Local Group. Assuming that the photometric mass estimate thus derived is fairly close to its dynamical mass, we predict that this GC has a (one-dimensional) velocity dispersion of the order of  (72 ± 13) km s⁻¹  . As a surviving 'super' star cluster, this object is of prime importance for theories aimed at describing massive star cluster evolution.     

Violent stellar merger model for transient events

We derive the constraints on the mass ratio for a binary system to merge in a violent process. We find that the secondary-to-primary stellar mass ratio should be  0.003 ≲ ( M ₂/ M ₁) ≲ 0.15  . A more massive secondary star will keep the primary stellar envelope in synchronized rotation with the orbital motion until merger occurs. This implies a very small relative velocity between the secondary star and the primary stellar envelope at the moment of merger, and therefore very weak shock waves, and low-flash luminosity. A too low-mass secondary will release small amount of energy, and will expel small amount of mass, which is unable to form an inflated envelope. It can, however, produce a quite luminous but short flash when colliding with a low-mass main-sequence star.
Violent and luminous mergers, which we term mergebursts, can be observed as V838 Monocerotis-type events, where a star undergoes a fast brightening lasting days to months, with a peak luminosity of up to  ∼10⁶ L_⊙  followed by a slow decline at very low effective temperatures.     

New age estimates of M31 globular clusters from multicolour photometry

The large majority of extragalactic star cluster studies performed to date essentially use multicolour photometry, combined with theoretical stellar synthesis models, to derive ages, masses, extinction estimates and metallicities. M31 offers a unique laboratory for studies of globular cluster (GC) systems. In this paper, we obtain new age estimates for 91 M31 GCs, based on improved photometric data, updated theoretical stellar synthesis models and sophisticated new fitting methods. In particular, we used photometric measurements from the Two Micron All Sky Survey (2MASS), which, in combination with optical photometry, can partially break the well-known age–metallicity degeneracy operating at ages in excess of a few Gyr. We show robustly that previous age determinations based on photometric data were affected significantly by this age–metallicity degeneracy. Except for one cluster, the ages of our other sample GCs are all older than 1 Gyr. Their age distribution shows populations of young- and intermediate-age GCs, peaking at ∼3 and 8 Gyr, respectively, as well as the 'usual' complement of well-known old GCs, i.e. GCs of similar age as the majority of the Galactic GCs. Our results also show that although there is significant scatter in metallicity at any age, there is a notable lack of young metal-poor and old metal-rich GCs, which might be indicative of an underlying age–metallicity relationship among the M31 GC population.     

断层平面组合样式对盆地砂体沉积的控制作用

利用三维地震、钻井、测井等资料,研究渤中凹陷石南断层和沉积体系展布,探讨断层平面组合样式对砂体的控制作用.结果表明:石南断层按走向不同可划分为6条分支断层,相邻分支断层在平面上相交构成"凹"型与"凸"型2种组合样式.研究区沙一+二段沉积期,发育辫状河三角洲、滨浅湖滩坝和湖泊等沉积相类型.在石臼坨凸起上发育多个物源供应方向,断层西端多个规模较小的物源可汇聚在一起,形成辫状河三角洲沉积,向湖盆中央延伸较远,规模较大;断层中部为主体物源供应方向,形成单个规模较大的辫状河三角洲沉积.在断层的"凹"型组合部位,容易形成主物源的进积方向,靠近盆地位置容易聚集砂体,在隆起区沿断层发育的古沟谷是碎屑物质进积的主要通道;在紧邻"凸"型组合样式的盆地区,难以形成较大规模的砂体沉积.该规律对寻找处于勘探初期含油气盆地砂砾岩储集层具有积极的意义.     

KSS31M型海洋重力仪在动、静态条件下观测到的读数变化及分析

2002年中国科学院海洋研究所从德国引进了KSS31M型海洋重力仪．为对该重力仪的工作性能有详细的了解,分别在德国重力仪生产厂实验室、中国科学院海洋研究所重力仪实验室进行了静态的定点观测,将重力仪安装在考察船上在黄埔江渔政码头等地进行了动态条件下的定点观测．动、静态的定点观测发现了多种规律性的重力仪读数变化,分析认为这些规律性的读数变化分别是重力仪的随机振荡、月潮的重力效应、海潮的重力效应和重力仪的线性漂移．它们各自有着不同的变化规律,并在海洋重力观测时总是同时存在．重力仪的随机振荡是重力仪自身固有的,其振荡幅度随外界条件的变化而变化,一般为0．04mGal～0．5mGal,周期为2～5min不等,在德国的重力仪厂家实验室和中国科学院海洋研究所重力实验室中观测到了月潮引起的重力变化,其变化幅度为0．2mGal．月潮引起的重力变化和海潮引起的重力变化同步,但相位相反．本文指出,仪器的月漂往往很难精确判定,本文用多种方法计算得到的仪器月漂在1．2mGal到2．3mGal之间．     

The X‐ray source population of the Andromeda galaxy M 31

First studies of the X‐ray source population of M 31 were performed with the Einstein Observatory and ROSAT. High resolution Chandra Observatory images not only spatially resolved the center area but also supernova remnants (SNRs) in the galaxy. Source catalogues of restricted areas were presented with high astrometric accuracy. Also luminosity function studies and studies of individual sources based on Chandra and XMM‐Newton observations led to a better knowledge of the X‐ray source population. An XMM‐Newton source catalog based on archival observations revealed more than 850 sources down to a 0.2–4.5 keV luminosity of 10³⁵ erg s^–1. EPIC hardness ratios as well as informations from earlier X‐ray, optical, and radio catalogues were used to distinguish between different source classes (SNRs, supersoft sources (SSSs), X‐ray binaries (XRBs), globular cluster sources within M 31, and foreground stars and objects in the background). However, many sources could only be classified as “hard”. These sources may either be XRBs or Crab‐like SNRs in M 31 or background sources. Two of the globular cluster sources could be identified as low mass XRBs with a neutron star as compact object as they showed type I X‐ray bursts. Many of the SSSs were identified as optical novae. Inspired by these results an XMM‐Newton survey of the entire D₂₅ disk of M 31 and a dedicated program to monitor X‐ray counterparts of optical novae in M 31 was started. We discuss implications for further nearby galaxy studies. (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

东营凹陷民丰地区沙三段中下亚段物源体系及其控储作用

民丰地区是东营凹陷油气勘探中的重要部分,其中物源体系分析对沉积体系研究及储层评价工作的开展具有重要意义。古地貌控制了沉积体系展布的基本格局,陈南断层下降盘、民丰洼陷腹部以及辛镇地区为砂体沉积提供了所需的可容纳空间。特征元素分析以及砂分散体系研究表明,沙三段中下亚段沉积时期,民丰地区发育了三大物源体系,沉积原始组分的供给主要来自北部陈家庄凸起、东部青坨子凸起以及南部盆外水系的注入。在该时期,辛镇地区F1、F2主断裂形成的构造调节带可作为南北向物源输送通道,东部物源体系控制下的沉积体系南端与南部盆外水系的北部分支于辛镇地区发生交汇。由于沉积原始组分是储层发育的基础,因此,不同物源体系控制下的沉积原始组分造成了储层储集空间及物性特征的差异性。混源区与东部物源控制下的储集体为三角洲前缘相带,弱压实,粒间原生孔发育,孔、渗性良好,优于南部以及北部物源体系控制下的储层物性,但南部储层含油性高于东部,混源区储层含油性最好。     

KSS31M型海洋重力仪动态性能的分析

采用海上实测数据对KSS31M(SN 036)海洋重力仪的阻尼延迟时间和可靠性做了分析,提出采用船只机动转向时重力数据和定位数据、厄特渥斯值的响应时间差来确定在该海况和仪器滤波系数时重力仪的阻尼延迟时间。得到的2级海况滤波系数下的阻尼延迟时间为60 s,比厂方提供的理论值更接近实际。本方法有助于提高海洋重力测量的精度。同时重力读数与厄特渥斯值变化的相位和振幅吻合,表明KSS31M海洋重力仪具有很高的可靠性和准确性。