Spectroscopic analysis of nearby lower-main-sequence stars     

X. M. Wang  J. R. Shi  G. Zhao 《Monthly notices of the Royal Astronomical Society》2009,399(3):1264-1274

Abundances of O, Na, Mg, Al, Si, K, Ca, Sc, Ti, V, Cr, Fe, Ni and Ba are determined for 30 nearby lower-main-sequence stars in the Northern sky using high-resolution, high signal-to-noise ratio spectra. Our results show an equilibrium of  [Fe/H]_I  and  [Fe/H]_II  and a much smaller star-to-star scatter of the abundance ratios as a function of metallicity compared with the results of Kotoneva et al. The non-local thermodynamic equilibrium (non-LTE) corrections for oxygen are considered and found to be small  (∼−0.04 dex)  . A flat trend of [O/Fe] exists over the whole metallicity range. The non-LTE effects for some important elements are discussed, and it is found that the abundance pattern for our programme stars is very similar to that of F and G dwarfs.  相似文献   

Tidal disruption of globular clusters in dwarf galaxies with triaxial dark matter haloes     

Jorge Peñarrubia  Matthew G. Walker  Gerard Gilmore 《Monthly notices of the Royal Astronomical Society》2009,399(3):1275-1292

We use N -body simulations to study the tidal evolution of globular clusters (GCs) in dwarf spheroidal (dSph) galaxies. Our models adopt a cosmologically motivated scenario in which the dSph is approximated by a static Navarro, Frenk & White halo with a triaxial shape. We apply our models to five GCs spanning three orders of magnitude in stellar density and two in mass, chosen to represent the properties exhibited by the five GCs of the Fornax dSph. We show that only the object representing Fornax's least dense GC (F1) can be fully disrupted by Fornax's internal tidal field – the four denser clusters survive even if their orbits decay to the centre of Fornax. For a large set of orbits and projection angles, we examine the spatial and velocity distribution of stellar debris deposited during the complete disruption of an F1-like GC. Our simulations show that such debris appears as shells, isolated clumps and elongated overdensities at low surface brightness (≥26 mag arcsec⁻²), reminiscent of substructure observed in several Milky Way dSphs. Such features arise from the triaxiality of the galaxy potential and do not dissolve in time. The kinematics of the debris depends strongly on the progenitor's orbit. Debris associated with box and resonant orbits does not display stream motions and may appear 'colder'/'hotter' than the dSph's field population if the viewing angle is perpendicular/parallel to the progenitor's orbital plane. In contrast, debris associated with loop orbits shows a rotational velocity that may be detectable out to a few kpc from the galaxy centre. Chemical tagging that can distinguish GC debris from field stars may reveal whether the merger of GCs contributed to the formation of multiple stellar components observed in dSphs.  相似文献   

Galaxies–intergalactic medium interaction calculation – I. Galaxy formation as a function of large-scale environment     

Robert A. Crain  Tom Theuns  Claudio Dalla Vecchia  Vincent R. Eke  Carlos S. Frenk  Adrian Jenkins  Scott T. Kay  John A. Peacock  Frazer R. Pearce  Joop Schaye  Volker Springel  Peter A. Thomas  Simon D. M. White  Robert P. C. Wiersma 《Monthly notices of the Royal Astronomical Society》2009,399(4):1773-1794

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Study of the dependence of the star formation rate in the nuclear regions of 39 Kazarian galaxies on their integral parameters     

V. Zh. Adibekyan  A. R. Petrosian 《Astrophysics》2009,52(2):192-204

A statistical study of the dependence of the star formation rate in the nuclear regions of 39 Kazarian galaxies on the integral parameters of these galaxies is carried out on the basis of spectra from SDSS DR6. The value of SFR/kpc² for our sample lies in the range 0.013÷2.04M _⨀ year⁻¹kpc⁻² (with the maximum value of 2.04 corresponding to the Kaz 98 (merger)). It is found that the surface density of the rate of star formation correlates positively with the bar structure parameter and EW(Hα), and that, for spiral galaxies of early morphological types, SFR/kpc² is greater than for the later types. It is shown that the color B-R for the galaxies and the color (u − g) _nucl for the nuclear region correlate positively with the total absorption A(Hα) in the Ha line for the nuclear region. The average value of A(Hα) for our samples is found to be A(Hα)=1.3±0.09 magnitudes. Translated from Astrofizika, Vol. 52, No. 2, pp. 211–224 (May 2009).  相似文献   

年轻星天体的质量     

尹佳  江治波 《天文学进展》2009,27(4)

质量是恒星最基本、最重要的物理量之一,它在恒星形成和演化过程中起着至关重要的作用.年轻星天体的形成机制以及早期演化过程是彻底解决恒星形成问题的关键所在,而年轻星天体形成过程中的物质下落、质量吸积以及外流等物理过程都与年轻星天体的质量密切相关.该文介绍了确定年轻星天体质量的一些常用方法,包括利用开普勒定律的动力学方法、赫罗图方法、年轻星天体脉动方法和磁层吸积方法等.并对这些方法的适用范围及测量精度进行了评述,还综述了各种方法的研究进展及未来可能的发展.  相似文献   

On a new cluster of H<Subscript>2</Subscript>O maser spots in the source ON2     

E. E. Lekht  A. M. Tolmachev  G. M. Rudnitskii 《Astronomy Letters》2009,35(2):132-135

We present the results of our observations of the H₂O maser emission toward the complex source ON2 associated with an active star-forming region. The observations were performed in a wide range of radial velocities, from ?75 to 90 km s^?1. We have detected an emission with flux densities of 9.2, 4, and 26 Jy at radial velocities of ?33.5, ?24.4, and ?18.8 km s^?1, respectively, at which no emission has been observed previously. The detected emission is most likely associated with a hitherto unknown cluster of maser spots located between the northern (N) and southern (S) components of the source ON2 (closer to the northern one). This cluster may be associated with one of the three CO molecular outflows in the ON2 region. We have also detected an emission at ?22 and ?14.5 km s^?1 in N and at 12.6 km s^?1 in S, which has extended significantly the velocity ranges of the maser emission in these sources and allowed their models to be improved.  相似文献   

A multiwavelength study of the massive star-forming region IRAS 22506+5944     

Yuan-Wei Wu  Ye Xu  Ji Yang  Jing-Jing Li 《中国天文和天体物理学报》2009,9(12)

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东昆仑西段祁漫塔格群的重新厘定   总被引：5，自引：0，他引：5  

王向利  高小平  刘幼骐  李新林  周小康  杜少喜  崔继刚  戴新宇  曾忠诚 《西北地质》2010,43(4):168-178

通过区域地质调查和研究,认为前人所建立的的祁漫塔格群或滩间山群包括了不同时代的浅变质碎屑岩、中酸性火山岩及基性-超基性岩。根据在东昆仑原划奥陶系祁漫塔格群第一亚群(下部碎屑浊积岩)中采集到早志留世笔石化石组合(这是首次证实东昆仑地区存在志留系地层)及同位素测年资料(鸭子大板火山岩年龄),其时代包含了奥陶纪、志留纪和三叠纪等,根据中国地层指南及中国地层指南说明书和地层清理,对祁漫塔格群进行了解体,将其重新厘定为奥陶纪滩间山群(OT)、志留纪白干湖岩组(Sb)弧后盆地复理石沉积和鸭子泉组(Sy)岛弧火山岩、石炭纪鸭子大坂硅质岩(S i)、三叠纪鄂拉山组(T3e)、蓟县纪狼牙山岩组(Jx l)和南华—奥陶纪阿牙克库木湖蛇绿混杂岩[(N h—O)aΣ]。该成果对于祁漫塔格地区早古生代地层划分对比、构造演化提供了重要新证据。  相似文献   

西秦岭北缘断裂宝鸡—武山段活动触发滑坡分布规律与成因机制     

辛鹏  吴树仁  张泽林  刘甲美  王涛  石菊松 《地质力学学报》2017,23(5):723-733

西秦岭北缘断裂沿"一带一路"交通廊道展布,是南北活动构造带强震丛集发育的节点之一,地震地质灾害风险极高。基于地质调查、测绘与数值分析,查明了断裂在天水地区触发的地震滑坡分布特征,探讨了断裂触发滑坡的形成机制。研究表明:(1)西秦岭北缘活动触发的巨、大型滑坡为断裂地貌过程的一部分,易在断裂的阶区聚集发育,其枢纽部位也有零星的分布;(2)巨大型滑坡集中于历史极震区内,断裂破裂过程中的近场惯性滑移、远场地震动是主要触发因素,二者耦合作用导致巨大型滑坡在断裂带两侧具有对称分布特征,活动强度由近及远而逐渐变弱;(3)断裂水平滑移、破裂引起的斜坡滑动变形以结构面贯通为主要表现形式,具有强烈的方向效应、近直立断层的区域地震动效应及地震波的山体地形放大效应,这些力学效应在滑坡破坏过程产生断裂结构面、次级羽裂结构面与滑动面,它们协同控制了滑坡的运动;(4)极端降雨触发的泥流是巨大型滑坡堆积体复活运动的主要形式,是现今防灾减灾重点。  相似文献   

Review of Deep-Penetrating Geochemical Exploration Methods     

Han Zhixuan  Liao Jianguo  Zhang Yulong  Zhang Bimin  Wang Xueqiu 《地球科学进展》2017,32(8):828-838

It is a worldwide challenge to explore the deeply buried deposits. Deep-penetrating geochemical exploration methods were developed to solve the problems of how to get the information of the buried deposits in the covered layer. The methods were successfully used to indicate some buried deposits, but not all kinds of deposits. What is more, a method cannot be used in all kinds of landscapes. In this paper, theories and case studies of deep-penetrating geochemical exploration methods, including mobile metal ions, enzyme leach, leaching of mobile forms of metals in overburden, electro-geochemical extraction method, biogeochemical exploration, nano-metal in geogas were reviewed. Elements migration, unloading mechanism and anomaly models are the most important parts for deep-penetrating geochemistry and need to be further investigated. From the perspective of economic efficiency and applicability, sampling and analyzing procedures should be simplified to improve the stability of all methods.  相似文献