The X-ray binary X2127+119 in M15: evidence for a very low mass, stripped-giant companion     

L. van Zyl  P. A. Charles  S. Arribas †  T. Naylor  E. Mediavilla  C. Hellier 《Monthly notices of the Royal Astronomical Society》2004,350(2):649-656

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A Chandra X-ray observation of the globular cluster Terzan 1   总被引：1，自引：0，他引：1  

E. M. Cackett  R. Wijnands  C. O. Heinke †  D. Pooley ‡  W. H. G. Lewin  J. E. Grindlay  P. D. Edmonds  P. G. Jonker  J. M. Miller 《Monthly notices of the Royal Astronomical Society》2006,369(1):407-415

We present a ∼19-ks Chandra Advanced CCD Imaging Spectrometer (ACIS)-S observation of the globular cluster Terzan 1. 14 sources are detected within 1.4 arcmin of the cluster centre with two of these sources predicted to be not associated with the cluster (background active galactic nuclei or foreground objects). The neutron star X-ray transient, X1732−304, has previously been observed in outburst within this globular cluster with the outburst seen to last for at least 12 yr. Here, we find four sources that are consistent with the ROSAT position for this transient, but none of the sources are fully consistent with the position of a radio source detected with the Very Large Array that is likely associated with the transient. The most likely candidate for the quiescent counterpart of the transient has a relatively soft spectrum and an unabsorbed 0.5–10 keV luminosity of  2.6 × 10³² erg s⁻¹  , quite typical of other quiescent neutron stars. Assuming standard core cooling, from the quiescent flux of this source we predict long (>400 yr) quiescent episodes to allow the neutron star to cool. Alternatively, enhanced core cooling processes are needed to cool down the core. However, if we do not detect the quiescent counterpart of the transient this gives an unabsorbed 0.5–10 keV luminosity upper limit of  8 × 10³¹ erg s⁻¹  . We also discuss other X-ray sources within the globular cluster. From the estimated stellar encounter rate of this cluster we find that the number of sources we detect is significantly higher than expected by the relationship of Pooley et al.  相似文献   

Mineralogy,nucleation and growth of dolomite in the laboratory and sedimentary environment: A review          下载免费PDF全文

Jay M. Gregg  David L. Bish  Stephen E. Kaczmarek  Hans G. Machel 《Sedimentology》2015,62(6):1749-1769

Dolomite [CaMg(CO₃)₂] forms in numerous geological settings, usually as a diagenetic replacement of limestone, and is an important component of petroleum reservoir rocks, rocks hosting base metal deposits and fresh water aquifers. Dolomite is a rhombohedral carbonate with a structure consisting of an ordered arrangement of alternating layers of Ca²⁺ and Mg²⁺ cations interspersed with anion layers normal to the c‐axis. Dolomite has symmetry, lower than the (CaCO₃) symmetry of calcite primarily due to Ca–Mg ordering. High‐magnesium calcite also has symmetry and differs from dolomite in that Ca²⁺ and Mg²⁺ ions are not ordered. High‐magnesium calcite with near‐dolomite stoichiometry (≈50 mol% MgCO₃) has been observed both in nature and in laboratory products and is referred to in the literature as protodolomite or very high‐magnesium calcite. Many dolomites display some degree of cation disorder (Ca²⁺ on Mg²⁺ sites and vice versa), which is detectable using transmission electron microscopy and X‐ray diffractometry. Laboratory syntheses at high temperature and pressure, as well as studies of natural dolomites show that factors affecting dolomite ordering, stoichiometry, nucleation and growth include temperature, alkalinity, pH, concentration of Mg and Ca, Mg to Ca ratio, fluid to rock ratio, mineralogy of the carbonate being replaced, and surface area available for nucleation. In spite of numerous attempts, dolomite has not been synthesized in the laboratory under near‐surface conditions. Examination of published X‐ray diffraction data demonstrates that assertions of dolomite synthesis in the laboratory under near‐ambient conditions by microbial mediation are unsubstantiated. These laboratory products show no evidence of cation ordering and appear to be very high‐magnesium calcite. Elevated‐temperature and elevated‐pressure experiments demonstrate that dolomite nucleation and growth always are preceded by very high‐magnesium calcite formation. It remains to be demonstrated whether microbial‐mediated growth of very high‐magnesium calcite in nature provides a precursor to dolomite nucleation and growth analogous to reaction paths in high‐temperature experiments.  相似文献   

Visualization of geologic geospatial datasets through X3D in the frame of WebGIS     

《International Journal of Digital Earth》2013,6(5):483-503

Abstract

3D geo spatial data have become the normal. However, to view the data, usually expert software is required, which have up to now hindered the wide spread use of 3D scenes for the display of geological data. The internet real time 3D rendering framework X3D is assessed regarding its suitability for building a geological GIS on the internet. Especially important for geological data, 3D rendering enhances the intuitive grasp of the data and enables the user to interactively explore it. It is often necessary to find a solution to distribute this data to a wide range of interested parties, experts and non-experts alike. According to the nature of 3D data, the best technique to display geo-data, the modeling of objects and unresolved issues have to be taken into consideration. The internet is the apparent tool for the public distribution and visualization of 3D data and it was found that through the open ISO-standardized format X3D it offers a multitude of possibilities. A 3D geological interactive map was created with these prerequisites to identify challenges and possibilities through this process. It was found that the use of lead to satisfactory results, that could probably not have been achieved with another technology.  相似文献   

南极乔治王岛六种苔藓植物的X荧光分析   总被引：5，自引：4，他引：5       下载免费PDF全文

黄宇营  巨新  康士秀  吴自勤  沈显生  孙立广  尹雪斌  张莉 《极地研究》2001,13(1):50-56

在无标样条件下 ,我们利用微束 X荧光分析法对南极乔治王岛的 6种苔藓植物的叶和茎进行重元素分析。它们是 :Andreaea regularis,Bryum muehlenbeckii,Drepanocladus uncinatus,Brachythecium subpilosum,Tortula saxiola,Ditrichum austro- georgicum。研究结果发现 ,不同苔藓植物对各种不同重元素的吸收能力不同 ,即使是同一种植物 ,叶和茎中的重元素成分也有差异。在 6种苔藓中 ,Andreaea regularis体内的重元素种类最少 ,但其对 Fe有较强的吸收。由于南极环境条件优越 ,在苔藓植物体内 ,尚未发现大量有毒重金属元素的存在  相似文献   

Where do the progenitors of millisecond pulsars come from?     

A. Taani  C.M. Zhang  M. Al‐Wardat  Y.H. Zhao 《Astronomische Nachrichten》2012,333(1):53-59

Observations of a large population of millisecond pulsars (MSPs) show a wide divergence in the orbital periods (from approximately hours to a few months). In the standard view, low‐mass X‐ray binaries (LMXBs) are considered as progenitors for some MSPs during the recycling process. We present a systematic study that combines different types of compact objects in binaries such as cataclysmic variables (CVs), LMXBs, and MSPs. We plot them together in the so called Corbet diagram. Larger and different samples are needed to better constrain the result as a function of the environment and formations. A scale diagram showing the distribution of MSPs for different orbital periods and the aspects for their progenitors relying on accretion induced collapse (AIC) of white dwarfs in binaries. Thus massive CVs (M ≥ 1.1 M_⊙) can play a vital role on binary evolution, as well as of the physical processes involved in the formation and evolution of neutron stars and their magnetic fields, and could turn into binary MSPs with different scales of orbital periods; this effect can be explained by the AIC process. This scenario also suggests that some fraction of isolated MSPs in the Galactic disk could be formed through the same channel, forming the contribution of some CVs to the single‐degenerate progenitors of Type Ia supernova. Furthermore, we have refined the statistical distribution and evolution by using updated data. This implies that the significant studies of compact objects in binary systems can benefit from the Corbet diagram.Observations of a large population of millisecond pulsars (MSPs) show a wide divergence in the orbital periods (from approximately hours to a few months). In the standard view, low‐mass X‐ray binaries (LMXBs) are considered as progenitors for some MSPs during the recycling process. We present a systematic study that combines different types of compact objects in binaries such as cataclysmic variables (CVs), LMXBs, and MSPs. We plot them together in the so called Corbet diagram. Larger and different samples are needed to better constrain the result as a function of the environment and formations. A scale diagram showing the distribution of MSPs for different orbital periods and the aspects for their progenitors re  相似文献   

A magnetic cycle of τ Bootis? The coronal and chromospheric view     

K. Poppenhaeger  H.M. Günther  J.H.M.M. Schmitt 《Astronomische Nachrichten》2012,333(1):26-29

τ Bootis is a late F‐type main sequence star orbited by a Hot Jupiter. During the last years spectropolarimetric observations led to the hypothesis that this star may host a global magnetic field that switches its polarity once per year, indicating a very short activity cycle of only one year duration. In our ongoing observational campaign, we have collected several X‐ray observations with XMM‐Newton and optical spectra with TRES/FLWO in Arizona to characterize τ Boo's corona and chromosphere over the course of the supposed one‐year cycle. Contrary to the spectropolarimetric reconstructions, our observations do not show indications for a short activity cycle (© 2011 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

Charge exchange in massive star‐forming regions     

T. Montmerle  L.K. Townsley 《Astronomische Nachrichten》2012,333(4):355-360

As a result of feedback from massive stars, via their intense winds and/or supernova explosions, massive star‐forming regions are entirely filled with hot, X‐ray emitting plasmas, which escape into the ambient ISM. As shown recently by Townsley et al. for several “extreme” cases (Carina, M17, NGC 3576, NGC 3603, 30 Dor), by way of large Chandra ACIS mosaics, extra, non‐thermal emission lines are present on top of the standard lines emitted by hot plasmas. Some of them are very close to lines characteristic of charge‐exchange reactions between the hot plasma and the cold surrounding material, suggesting that this mechanism operates on large spatial scales (several 10 pc) in star‐forming regions in general. The connection with starburst galaxies is briefly mentioned, and it is pointed out that supernovae interacting with molecular clouds may also provide a good environment to look for charge exchange processes (© 2012 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

顾及不确定因素的GA-BP神经网络在路基沉降预测中的应用     

杨发群  邱卫宁  魏成  李成贤 《测绘工程》2013,(6):51-54

BP神经网络初始权值和阈值输入不同,将导致BP神经网络预测不稳定,精度也不是很高.通过遗传算法（GA）对BP神经网络的初始权值和阈值进行优化,能很大程度上提高预测的精度,但是,由于输入层不可能将影响输出的所有因素都包含在内,而这些没有考虑到的因素势必影响预测结果.文中将这些无法得知的不确定因素当做一个综合影响因素,定义为X因素,在建立模型时加以考虑.实验结果表明,这种顾及不确定因素的GA-BP神经网络模型能进一步提高预测精度.  相似文献   

蒙古国东南部钨多金属靶区的快速圈定与成矿分析     

黄雪飞  张宝林  贾文臣  李晓利  沈晓丽  郭志华 《地质与勘探》2012,48(5):906-914

复杂地表条件下矿产勘探一直是个难题,国外区块更是如此,首次利用XLT一592WZ型便携式XRF分析仪在蒙古国苏赫巴托尔省（额尔德尼查干苏木）13451X草原覆盖地区系统采集数据,分析研究并圈定成矿靶区。初期利用x荧光仪进行扫面勘探,发现有W、As、Ph、Zn、Cu、Fe等元素异常,经过异常查证优选了一个钨多金属找矿远景区。在钨多金属找矿远景区内通过23条探槽和钻探工程进一步揭露发现一条黑钨矿体;钨矿主要以脉状、团块状或是角砾状形式出现,成矿围岩为花岗斑岩,矿石以黑钨矿为主,白钨矿极少,可见硅化、萤石,推测该区成矿类型为高温热液型黑钨矿。综合来看,在野外利用便携式X荧光光谱仪进行定性与半定量分析是有效的,该方法可在同类地区推广应用。  相似文献