X-ray Raman scattering for structural investigation of silica/silicate minerals     

H. Fukui  M. Kanzaki  N. Hiraoka  Y. Q. Cai 《Physics and Chemistry of Minerals》2009,36(3):171-181

We have performed X-ray Raman scattering (XRS) measurements on the oxygen K and silicon L absorption edges of four silica minerals: α-quartz, α-cristobalite, coesite, and stishovite. We have also calculated the partial electron densities of states (DOSs) and compared these with the XRS spectra. This study demonstrates that the short-range structure around the atom of interest strongly influences the XRS spectral features. Importantly, the oxygen K-edge XRS spectra are found to reflect the p-orbital DOS while the silicon L-edge spectra reflect the s- and d-orbital DOSs, even when a product of a momentum transfer and a mean radius of a electron orbit (1s for oxygen and 2p for silicon), Qr, is close to or larger than unity. Building on this, calculations of the partial DOSs for other silica phases are presented, including ultra-high-pressure phases, which provide a good reference for further XRS study of silica and silicate minerals. XRS measurements should be performed on not only either of oxygen or silicon but also on many kinds of constituent elements to reveal the structural change of glasses/melts of silicates under extreme conditions.  相似文献   

钾含量对白云母X射线衍射特征的影响   总被引：5，自引：1，他引：4  

王德强  王辅亚  王冠鑫  张惠芬 《大地构造与成矿学》2004,28(1):69-73

对白云母X射线衍射峰强度的理论计算,发现其衍射峰的强度随钾含量呈规律性变化;对白云母活化释钾后不同钾含量样品进行X射线衍射实验,发现实测的衍射峰强度值与计算值变化趋势一致。计算与实测的白云母特征衍射峰强度比值曲线也有相同的变化趋势。这些结果表明白云母中钾含量是其X射线衍射特征变化的主要原因。  相似文献   

Calculation of the Intensity Ratio and Intrinsic Redshift Ratio of the Cerenkov Iron K_α and K_β Lines and Its Possible Application in the Study of AGNs     

Dang-bo Liu  Lei Chen  Jun-han You 《Chinese Astronomy and Astrophysics》2008

We have pointed out that, when thermal relativistic electrons with an isotropic velocity distribution move through a region of dense gas or impinge upon its surface, the Cerenkov effect will produce a particular kind of atomic or ionic emission line, which we have called the “Cerenkov line-like radiation”. This prediction for the optical wavebands has been verified by laboratory experiments. In this paper, we extend this line-like radiation theory to the X-ray waveband and give the basic formulae for calculating the intensity ratio and intrinsic redshift ratio of the Cerenkov iron K_α and K_β lines, for different ionization orders of iron. Potential application of this calculated result may be found in the study of AGNs. The recent observations of NGC3783 show that besides the iron K_α line at ∼6.4 keV, there is also a very strong iron Kβ line at ∼7.0 keV, and that the ratio of equivalent widths between the two is anomalous: EWK_α/EWK_β ≈ 3.43. It is difficult to explain this by the conventional mechanism of “photoelectric absorption-fluorescence emission”. We suggest that the mechanism of Cerenkov line-like radiation can provides a way of solving this puzzle. Besides, we expect that the calculated intrinsic redshift ratio of Cerenkov iron K_α and K_β lines could be tested in future observations. If our suggestion is further supported by observations, then our view on the physical environment around the central massive black hole of an AGN will be greatly modified: the activity becomes more energetic and violent, and the gas, much denser than previously thought.  相似文献   

New active galactic nuclei among the INTEGRAL and SWIFT X-ray sources     

R. A. Burenin  A. V. Mescheryakov  M. G. Revnivtsev  S. Yu. Sazonov  I. F. Bikmaev  M. N. Pavlinsky  R. A. Sunyaev 《Astronomy Letters》2008,34(6):367-374

We present the results of our optical identifications of a set of X-ray sources from the INTEGRAL and SWIFT all-sky surveys. The optical data have been obtained with the 1.5-m Russian-Turkish Telescope (RTT-150). Nine X-ray sources have been identified with active galactic nuclei (AGNs). Two of them are located in the nearby spiral galaxies MCG-01-05-047 and NGC 973 seen almost edge-on. One source, IGR J16562-3301, is probably a BL Lac object (blazar). The remaining AGNs are observed as the starlike nuclei of spiral galaxies whose spectra exhibit broad emission lines. The relation between the hard X-ray (17–60 keV) luminosity and the [O III] 5007 line luminosity, log L _x/L _{[O III]} ≈ 2.1, holds good for most of the AGNs detected in hard X rays. However, the luminosities of some AGNs deviate from this relation. The fraction of such objects can reach ～20%. In particular, the [O III] line flux is lower for two nearby edge-on spiral galaxies. This can be explained by the effect of absorption in the galactic disks.  相似文献   

Optical identifications of five INTEGRAL hard X-ray sources in the Galactic plane     

I. F. Bikmaev  R. A. Burenin  M. G. Revnivtsev  S. Yu. Sazonov  R. A. Sunyaev  M. N. Pavlinsky  N. A. Sakhibullin 《Astronomy Letters》2008,34(10):653-663

The results of optical identifications of five hard X-ray sources in the Galactic plane from the INTEGRAL all-sky survey are presented. The X-ray data on one source (IGR J20216+4359) are published for the first time. The optical observations were performed with the 1.5-m RTT-150 telescope (Turkish National Observatory, Antalya, Turkey) and the 6-m BTA telescope (Special Astrophysical Observatory, Nizhny Arkhyz, Russia). A blazar, three Seyfert galaxies, and a high-mass X-ray binary are among the identified sources.  相似文献   

Diagnostics of the early explosion phase of a classical nova using its X-ray emission: A model for the X-ray outburst of CI Camelopardalis in 1998     

E. V. Filippova  M. G. Revnivtsev  A. A. Lutovinov 《Astronomy Letters》2008,34(12):797-819

We have computed a spherically symmetric model for the interaction of matter ejected during the outburst of a classical nova with the stellar wind from its optical component. This model is used to describe the intense X-ray outburst (the peak 3–20 keV flux was ～2 Crab) of the binary system CI Camelopardalis in 1998. According to our model, the stellar wind from the optical component heated by a strong shock wave produced when matter is ejected from the white dwarf as the result of a thermonuclear explosion on its surface is the emission source in the standard X-ray band. Comparison of the calculated and observed time dependences of the mean radiation temperature and luminosity of the binary system during its outburst has yielded very important characteristics of the explosion. We have been able to measure the velocity of the ejected matter immediately after the onset of the explosion for the first time: it follows from our model that the ejected matter had a velocity of ～2700 km s^?1 even on 0.1–0.5 day after the outburst onset and it flew with such a velocity for the first 1–1.5 day under an external force, possibly, the radiation pressure from the white dwarf. Subsequently, the matter probably became transparent and began to decelerate. The time dependence of the mean radiation temperature at late expansion phases has allowed us to estimate the mass of the ejected matter, ～10^?7–10^?6 M _⊙. The mass loss rate in the stellar wind required to explain the observed peak luminosity of the binary system during its outburst has been estimated to be \(\dot M\) ～ (1 ? 2) × 10^?6 M _⊙ yr^?1.  相似文献   

ADAFs, accretion discs and outbursts in compact binaries     

Jean-Pierre Lasota   《New Astronomy Reviews》2008,51(10-12):752

I discuss the status of the soft X-ray transient model. First, I discuss and then compare with observations the assumption that the geometrically thin disc evaporates into an ADAF. Second, I address the problems created by the recent determinations of the distance to SS Cyg, according to which the disc instability model does not apply to this famous dwarf-nova, thus casting doubt on the application of this model to any system at all.  相似文献   

Fast rotation of neutron stars and equation of state of dense matter     

Pawe&#x; Haensel  Julian L. Zdunik  Micha&#x; Bejger 《New Astronomy Reviews》2008,51(10-12):785

Fast rotation of compact stars (at sub-millisecond period) and, in particular, their stability, are sensitive to the equation of state (EOS) of dense matter. Recent observations of XTE J1739-285 suggest that it contains a neutron star rotating at 1122 Hz. At such rotational frequency the effects of rotation on star’s structure are significant. We study the interplay of fast rotation, EOS, and gravitational mass of a sub-millisecond pulsar. We discuss the EOS dependence of spin-up to a sub-millisecond period, via mass accretion from a disk in a low-mass X-ray binary.  相似文献   

射电选和X射线选BL Lacertae天体的射电性质   总被引：1，自引：0，他引：1  

杨富利  李岳黄  杨江河 《天文研究与技术》2008,5(3)

收集了射电选和X射线选BL Lac天体的射电数据(包括核和延展光度), 并计算了它们的核主导系数R.研究显示: 射电选BL Lac(RBLs)天体的总射电光度是X射线选BL Lac(XBLs)天体的2个量级.详细分析得到这种差别主要是来自于核光度的差别因为延展光度差别只有1个量级.研究RBLs和XBLs的核(延展元)光度与核主导系数之间的关系, 发现延展元光度与核主导系数负相关, 而核(总)光度几乎与核主导系数没有相关.  相似文献   

X荧光光谱分析技术在测定安徽月山矿床铁铜矿石中Fe、Cu的应用研究     

刘春  郑洪涛  梁述廷  刘玉纯  安乐生 《矿物岩石地球化学通报》2019,(1):169-175

为建立符合安徽月山矿区的X荧光光谱(XRF)分析方法,针对矿区铁矿、铜矿的特点,用铁、铜矿石的国家标准物质制作系列校准样片,通过粉末压片和玻璃熔融两种制样方法,波长色散X荧光光谱法测定主矿体样品中的Fe、Cu等主量元素,并将测定结果与传统化学方法分析结果进行比较。结果显示,熔片法-XRF的测定结果与化学容量法测定结果一致,试样在850℃灼烧,按40∶1大稀释比熔融制样,解决了样品在高温熔融过程中对铂黄坩埚的腐蚀,适用于月山矿区铁铜矿样品中Fe、Cu的测定。粉末压片法不能克服矿物效应和粒度效应的影响,测定结果与化学容量法结果比对偏差较大,不适用于月山地区铁铜矿中Fe、Cu的测定。  相似文献