华北燕山造山带结构要素组合

采用造山带结构要素组合的概念,对华北燕山造山带进行了研究。燕山造山带各演化阶段的结构要素组合特征如下：前造山和初始造山幕(J1),早侏罗世早期为前造山伸展构造,结构要素组合有：三又式裂谷带、板内型玄武岩、含煤建造;早侏罗世晚期为初始造山收缩构造,结构要素组合有：向北倾伏的褶曲与逆冲、九龙山组类磨拉石建造,硬绿泥石一十字石一蓝晶石为标志的低温、中一高压变质带。早期造山幕(J2),中侏罗世早期为同造山伸展构造,结构要素组合有：岩石圈上隆伸展有关的火山盆地及可能的同期侵入岩,火山岩线型分布;中侏罗世晚期为收缩构造,有关的结构要素组合为：逆冲推覆和褶曲变形、磨拉石建造、同构造侵入体和角闪岩相变质岩。峰期造山幕(J3),晚侏罗世早期同构造伸展构造,结构要素组合有：岩石圈上隆伸展有关的火山盆地与同期侵入岩,火山岩面型分布,火成岩组合中出现高压粗面岩类,较大量的流纹岩;晚侏罗世晚期收缩构造有关结构要素组合为：逆冲推覆和褶曲变形、磨拉石建造、同构造侵入体和角闪岩相变质岩,侵入岩中出现高压正长岩类。早白垩世早期(K1^1)晚造山幕有关的结构要素组合为：收缩变形分布较局限,湖相沉积建造替代磨拉石建造,侵入岩组合中出现过碱性石英正长岩,大晶洞构造的花岗岩及科马提质辉长岩等。早白垩世晚期(K1^2)后造山幕伸展有关的结构要素组合为：正断层、变质核杂岩、双峰式岩墙辟、典型的过碱性花岗岩和含煤建造。     

滇西三江造山带中南段地球化学分区特征

正中国多类型区域地球化学调查工作获得了丰富的数据资源,其提供的全方位信息亦在矿产资源勘查等方面发挥了重要作用(Wang Xueqiu et al.,2007)。近年来,学者们尝试利用区域性化探数据进行元素的地球化学分区,取得了较好的效果(汤金来等,2016)。三江造山带是我国重要的成矿带之一,其区域化探工作始于上世纪60年代,并阶段性完成了1:50万、1:25万和1:20万多尺度     

The Monitor project: rotation of low-mass stars in NGC 2362 – testing the disc regulation paradigm at 5 Myr

We report on the results of a time-series photometric survey of NGC 2362, carried out using the CTIO 4-m Blanco telescope and Mosaic-II detector as part of the Monitor project. Rotation periods were derived for 271 candidate cluster members over the mass range  0.1 ≲ M /M_⊙≲ 1.2  . The rotation period distributions show a clear mass-dependent morphology, qualitatively similar to that in NGC 2264, as would be expected from the age of this cluster. Using models of angular momentum evolution, we show that angular momentum losses over the ∼1–5 Myr age range appear to be needed in order to reproduce the evolution of the slowest rotators in the sample from the ONC to NGC 2362, as found by many previous studies. By incorporating Spitzer IRAC mid-infrared (mid-IR) measurements, we found that three to four objects showing mid-IR excesses indicative of the presence of circumstellar discs were all slow rotators, as would be expected in the disc regulation paradigm for early pre-main-sequence angular momentum evolution, but this result is not statistically significant at present, given the extremely limited sample size.     

Haplosyllis spongicola Grube Polychaeta, Syllidae Associated with Two Species of Sponges from East Africa Tanzania, Indian Ocean

Abstract. The presence of Haplosyllis spongicola G rube 1855 Polychaeta, Syllidae in two sponge species from the Indian Ocean Tanzania, Theonella swinhoei G ray 1868 and Liosina paradoxa THIELE 1899, was detected. Polychaetes lived exclusively inside the aquiferous system of the sponges, reaching a mean density of 68 individuals · cm^-3 in T. swinhoei and 148 individuals · cm^-3 in L. paradoxa Acetone extractions were prepared from sponge tissues of T. swinhoei and L. paradoxa and from the gut contents of their respective inhabiting polychaetes. Absorption spectra matched for each sponge/polychaete pair. These data confirm that polychaetes exploit the soft parts of the sponges in which they live. In addition, in L. paradoxa direct confirmation of a predatory activity of worms on sponge internal tissues was obtained on the basis of the finding of terrigenous sediments, which typically reinforced the sponge canal walls, in the gut lumen of the inhabiting polychaete. No evident ultrastructural changes of the host tissue due to endobionts have been observed. These results confirm the parasitic/micropredatory habits of H. spongicola. Data on different morphological characteristics of H. spongicola living in the two sponge species are presented and discussed.     

Infrared photometry of low-mass stars in Praesepe

We present follow-up infrared photometry for a sample of low-mass and very low-mass stars in the Praesepe open cluster. Our sample is selected from two sources: (i) 90 stars selected from the Hambly et al. photometric and proper-motion survey of Praesepe; (ii) 17 stars selected from the CCD imaging survey presented by Pinfield et al. We investigate cluster membership using infrared colour–magnitude and colour–colour diagrams. We find 81 likely and two possible members in the Hambly et al. sample, in line with predictions. Contamination in the Pinfield et al. sample is higher, and we find nine probable cluster members. We investigate the non-grey models of Baraffe et al., which are found to be in good agreement with the data. Multiplicity in Praesepe is also examined, and we find the multiple star fraction to be 0.51 from analysis of the I , I − K diagram. We investigate individual object masses, and find that the faintest candidate cluster members have masses close to the substellar limit.     

A New Method of Open Cluster Membership Determination

Membership determination is the key-important step to study open clusters, which can directly in?uence on the estimation of open clusters’ physical parameters. DBSCAN (Density Based Spatial Clustering of Applications with Noise) is a density-based clustering algorithm in data mining techniques. In this paper the DBSCAN algorithm has been used for the ?rst time to make the membership determination of the open clusters NGC 6791 and M 67 (NGC 2682). Our results indicate that the DBSCAN algorithm can effectively eliminate the contamination of ?eld stars. The obtained member stars of NGC 6791 exhibit clearly a doubled main-sequence structure in the color-magnitude diagram, implying that NGC 6791 may have a more complicated history of star formation and evolution. The clustering analysis of M67 indicates the presence of mass segregation, and the distinct relative motion between the central part and the outer part of the cluster. These results demonstrate that the DBSCAN algorithm is an effective method of membership determination, and that it has some advantages superior to the conventional kinematic method.     

Single star scattering on an open cluster

We examine the scattering of single stars from an open star cluster. The probability of the capture of a star by a star cluster is dependent on the velocity and mass of the star, and the stars that are not captured experience a velocity change. For low-velocity stars there is an exponential decrease of the capture probability with the initial velocity, and the velocity change decreases almost linearly. For high-velocity stars there is a v ⁻⁶ dependence for the capture probability, and a v ⁻¹ dependence for the velocity change. Analytical estimations, Monte Carlo and full N -body simulations are all in good agreement.