欧空局的“多镜面X射线观测卫星”

“多镜面Ｘ射线观测卫星”（ＸＭＭ）是欧空局的新一代科学卫星。为欧空局研制这颗卫星的主承包商是德国的道尼尔卫星系统有限公司（ＤＳＳ），参予研制和制造该卫星的还有德国的戴姆勒－奔驰宇航公司和欧洲其他３５家公司，计划于１９９９年年中完成ＸＭＭ的研制工作。这...

X射线轫致辐射厚靶模型的改进及其在太阳耀斑观测中的应用

本文主要讨论对不同电离度分布厚靶模型的改进以及在耀斑X射线观测中推导非热电子、电离度和靶密度分布的应用．

球载X射线探测器观测目标自动跟踪系统

介绍一种基于ＧＰＳ卫星定位接收机的球载Ｘ射线探测器观测目标自动跟踪系统，包括以８０Ｃ１９６ＭＣＵ为核心的ＣＰＵ主板和数字Ｉ／Ｏ接口板，给出了程序流程和实验结果。此系统实现了对Ｘ射线天体的精确自动跟踪。

X射线天文观测卫星ASTRO-E的安全保障控制系统

1 前言ASTRO-E是X射线天文观测卫星,预定于2000年2月发射。该卫星载有用做观测仪器的X射线望远镜。从性质上来说,X射线难以弯曲,因此焦距长。为实现高性能X射线望远镜,ASTRO-E卫星在轨道上利用EOB(可伸展光学试验台)将望远镜筒部伸展开。展开后卫星本体全长达6.5m。随着伸展,与重量相比,卫星具有较大的惯性矩,承受较大的重力梯度力矩。该ASTRO-E卫星具有独特的安全保障(Safe-hold)控制系统,最适于强干扰的环境。现就该系统的设计概念、动力学。

Wolter-Ⅰ型X射线天文望远镜的光学设计

针对国内硬X射线天文观测的需求,研究了1～30keV能段圆锥嵌套Wolter-Ⅰ型X射线天文望远镜的光学设计,推导了嵌套层之间的结构递推关系,给出了合理的望远镜初始结构。在最内层和最外层之间,设计了6组W/B4C宽带非周期多层膜,模拟得到系统的有效集光面积和分辨力。理论有效集光面积达到127cm2(在2keV处)和71cm2(在30keV处),系统角分辨力约10″。系统实际成像质量还受到公差的影响,引起像质下降的公差主要有辐条位置公差、镜面位置公差和镜面面形公差。目前演示实验方便改善的公差是辐条位置公差,给出了此公差的计算方法并对系统进行光线追迹,得到了成像点列图和分辨力改变情况。辐条位置公差从±15μm缩小到±3μm后,系统分辨力由1′提高到13″。

Combining optical and X-ray observations of galaxy clusters to constrain cosmological parameters

Galaxy clusters present unique advantages for cosmological study.Here we collect a new sample of 10 lensing galaxy clusters with X-ray observations to constrain cosmological parameters.The redshifts of the lensing clusters lie between 0.1 and 0.6,and the redshift range of their arcs is from 0.4 to 4.9.These clusters are selected carefully from strong gravitational lensing systems which have both X-ray satellite observations and optical giant luminous arcs with known redshifts.Giant arcs usually appear in the central region of clusters,where mass can be traced with luminosity quite well.Based on gravitational lensing theory and a cluster mass distribution model,we can derive a ratio using two angular diameter distances.One is the distance between lensing sources and the other is that between the deflector and the source. Since angular diameter distance relies heavily on cosmological geometry,we can use these ratios to constrain cosmological models.Moreover,X-ray gas fractions of galaxy clusters can also be a cosmological probe.Because there are a dozen parameters to be fitted,we introduce a new analytic algorithm,Powell's UOBYQA(Unconstrained Optimization By Quadratic Approximation) ,to accelerate our calculation.Our result demonstrates that this algorithm is an effective fitting method for such a continuous multi-parameter constraint.We find an interesting fact that these two approaches are separately sensitive toΩΛandΩM.By combining them,we can get reasonable fitting values of basic cosmological parameters:ΩM=0.26 +0.04 -0.04,andΩΛ=0.82 +0.14 -0.16.

XMM-Newton observations of H_2O maser galaxy NGC 7479

The XMM-Newton observations of H2O megamaser galaxy NGC 7479 are presented. Its smoothed X-ray image clearly shows spiral morphology, which matches well with its optical asymmetric spiral structure. One prominent source can be found at the tip of its northern spiral arm, which is much brighter than its nuclear X-ray source (about a 50% higher count rate). For the nuclear source (a circular region with a radius of 20 ), the spectra show soft excess below 2 keV and a strong iron Kα emission line. The best fitting model includes a partially absorbed model for the hard continuum and one thermal plasma model for the soft scatter component. Both the high column density (NH ～ 6.88×1023 cm-2) and strong fluorescent iron line (with an equivalent width of ～1.5 keV) support the existence of one heavily obscured AGN. For the bright prominent source, its radial profile is consistent with that of a single point-like source. Its spectra are extracted from the circular region around its peak, with a radius of 20 and 6 respectively and both spectra show no significant difference. Four alternative models for the ultra-luminous X-ray source (ULXs) can reproduce the spectra well: an absorbed power law, thermal bremsstrahlung, multicolor blackbody disk plus another blackbody or power law. Further observations (e.g., the tremendous improvement in the spatial resolution of the Chandra X-ray observations) and studies are desirable for probing the nature of this prominent source. In addition, we also estimate the mass of its central engine to be 1.18×107 M and maser disk parameters: the disk radius of ～0.7pc and the dimensionless accretion rate (L2-10keV/LEdd) of 1.2×10-4.

A possible mechanism for magnetar soft X-ray/γ-ray emission

Once the energies of electrons near the Fermi surface obviously exceed the threshold energy of the inverse β decay,electron capture(EC) dominates inside the magnetar.Since the maximal binding energy of the 3 P 2 neutron Cooper pair is only about 0.048 MeV,the outgoing high-energy neutrons(E k(n) > 60 MeV) created by the EC can easily destroy the 3 P 2 neutron Cooper pairs through the interaction of nuclear force.In the anisotropic neutron superfluid,each 3 P 2 neutron Cooper pair has magnetic energy 2μ n B in the applied magnetic field B,where μ n = 0.966 × 10 23 erg.G 1 is the absolute value of the neutron abnormal magnetic moment.While being destroyed by the high-energy EC neutrons,the magnetic moments of the 3 P 2 Cooper pairs are no longer arranged in the paramagnetic direction,and the magnetic energy is released.This released energy can be transformed into thermal energy.Only a small fraction of the generated thermal energy is transported from the interior to the surface by conduction,and then it is radiated in the form of thermal photons from the surface.After highly efficient modulation within the star's magnetosphere,the thermal surface emission is shaped into a spectrum of soft X-rays/γ-rays with the observed characteristics of magnetars.By introducing related parameters,we calculate the theoretical luminosities of magnetars.The calculation results agree well with the observed parameters of magnetars.

Development of the super high angular resolution principle for X-ray imaging

Development of the Super High Angular Resolution Principle (SHARP) for coded-mask X-ray imaging is presented. We prove that SHARP can be considered as a generalized coded mask imaging method with a coding pattern comprised of diffraction-interference fringes in the mask pattern. The angular resolution of SHARP can be improved by detecting the fringes more precisely than the mask's element size, i.e. by using a detector with a pixel size smaller than the mask's element size. The proposed mission SHARP-X for solar X-ray observations is also briefly discussed.

X-ray spectroscopy of clusters of galaxies

Clusters of galaxies are the most massive objects in the Universe and precise knowledge of their mass structure is important to understand the history of structure formation and constrain still unknown types of dark contents of the Universe. X-ray spectroscopy of galaxy clusters provides rich information about the physical state of hot intracluster gas and the underlying potential structure. In this paper, starting from the basic description of clusters under equilibrium conditions, we review properties of clusters revealed primarily through X-ray observations considering their thermal and dynamical evolutions. The future prospects of cluster studies using upcoming X-ray missions are also mentioned.

The study of Seyfert 2 galaxies with and without infrared broad lines

From the literature, we construct a sample of 25 Seyfert 2 galaxies (S2s)with a broad line region (BLR) detected in near infrared (NIR) spectroscopy and 29with NIR BLRs which were not detected. We find no significant difference betweenthe nuclei luminosity (extinction-corrected [OIII] 5007) and infrared color f 60/f25between the two populations, suggesting that the non-detections of NIR BLRs couldnot be due to low AGN luminosity or contamination from the host galaxy. As ex-pected, we find significantly lower X-ray obscurations in Seyfert 2s with NIR BLRdetection, supporting the unification scheme. However, such a scheme was challengedby the detection of NIR BLRs in heavily X-ray obscured sources, especially in sixof them with Compton-thick X-ray obscuration. The discrepancy could be solved bythe clumpy torus model and we propose a toy model demonstrating that IR-thin X-ray-thick S2s could be viewed at intermediate inclinations and compared with thoseIR-thick X-ray-thick S2s. We note that two of the IR-thin X-ray-thick S2s (NGC 1386and NGC 7674) experienced X-ray transitions, i.e. from Compton-thin to Compton-thick appearance or vice versa based on previous X-ray observations, suggesting thatX-ray transitions could be common in this special class of objects.

低温相偏硼酸钡单晶的不完整性

对熔剂法生长的低温相偏硼酸钡(BBO)单晶的不完整性进行了X射线衍射形貌术观测和研究。主要的结构缺陷有钉扎较严重的位错、位错环、包裹物、丝状物、电峙和晶界等,并且简单地讨论了它们的可能成因。

The gamma-ray Doppler factor determinations for a Fermi blazar sample

Observations suggest that γ-ray loud blazars are strongly beamed. The Fermi mission has detected many of blazars, which provide us with a good oppor- tunity to investigate the emission mechanism and the beaming effect in the γ-ray re- gion. We compiled the X-ray observations for 138 Fermi blazars (54 flat spectrum radio quasars, 36 low-peaked BL Lacertae objects, and 48 high-peaked BL Lacertae objects) and calculated their Doppler factors, δγ . It is interesting that the calculated Doppler factors, δγ , are strongly correlated with the γ-ray luminosity.

The lower limit of the Doppler factor for a Fermi blazar sample

We selected 457 blazars(193 flat spectrum radio quasars, 61 lowsynchrotron peaked blazars, 69 intermediate-synchrotron peaked blazars and 134high-synchrotron peaked blazars) from the second Fermi-LAT catalog(2FGL) of γ-ray sources, which have X-ray observations. We calculated the lower limits for their Doppler factors, δγ, and compared the lower limits with the available Doppler factors and the apparent superluminal velocities in the literature.

Rescuing the intracluster medium of NGC 5813

We use recent X-ray observations of the intracluster medium(ICM) of the galaxy group NGC 5813 to confront theoretical studies of ICM thermal evolution with the newly derived ICM properties.We argue that the ICM of the cooling flow in the galaxy group NGC 5813 is more likely to be heated by mixing of post-shock gas from jets residing in hot bubbles with the ICM,than by shocks or turbulentheating.Shocks thermalize only a small fraction of their energy in the inner regions of the cooling flow;in order to adequately heat the inner part of the ICM,they would overheat the outer regions by a large factor,leading to its ejection from the group.Heating by mixing,which was found to be much more efficient than turbulent-heating and shocks-heating,hence,rescues the outer ICM of NGC 5813 from its predestined fate according to cooling flow feedback scenarios that are based on heating by shocks.

Inverse Optimizing Method of Bio-Temperature-Field Reconstruction in rf-Capacitive Hyperthermia

We propose an inverse optimizing method, used in rf-capacitive hyperthermia to obtain a certain target tumour temperature and to avoid the over-heating of normal tissues. Based on the finite-element-method solutions of the Laplace electric potential equation and Penne's bio-heat transfer equation, the heating conditions are modified by the genetic algorithms recursively to minimize the objective function for searching an optimum physical configuration. With a simplified human tissue model extracted from an x-ray computed tomography slice which has deep- and shallow-seated turnouts, satisfactory simulation results are obtained both on bi-plate and three-plate systems, e.g. The tumour temperature is higher than 43℃ and the temperature of normal tissues is lower than 39℃. It is suggested that the proposed algorithm is snitable for both shallow and deep seated cancer oncology.

Fractal dimension and thermodynamic fluctuation properties of IDV light curves

Fractals are a basic tool for phenomenologically describing natural objects having a high degree of temporal or spatial variability.From a physical point of view the fractal properties of natural systems can also be interpreted by using the standard formalism of thermodynamical fluctuations.We introduce and analyze the fractal dimension of the Intra-Day-Variability (IDV) light-curves of BL Lac objects,in the optical,radio and X-ray bands.A general description of the fluctuation spectrum of these systems based on general thermodynamical principles is also proposed.Based on the general fractal properties of a given physical system,we also introduce the predictability index for the IDV light curves.We have explicitly determined the fractal dimension for the R-band observations of five blazars,as well as for the radio band observations of the compact extragalactic radio source J 1128+5925 and of several X-ray sources.Our results show that the fractal dimension of the optical and X-ray observations indicates an almost pure "Brownian noise" (random walk) spectrum,with a very low predictability index,while in the radio band the predictability index is much higher.We have also studied the spectral properties of the IDV light curves and we have shown that their spectral index is very closely correlated with the corresponding fractal dimension.

A note on the puzzling spindown behavior of the Galactic center magnetar SGR J1745-2900

SGR J1745-2900 is a magnetar near the Galactic center. X-ray observations of this source found a decreasing X-ray luminosity accompanied by an enhanced spindown rate. This negative correlation between X-ray luminosity and spindown rate is hard to understand. The wind braking model of magnetars is employed to explain this puzzling spindown behavior. During the release of magnetic energy of magnetars,a system of particles may be generated. Some of these particles remain trapped in the magnetosphere and may contribute to the X-ray luminosity. The rest of the particles can flow out and take away the rotational energy of the central neutron star. A smaller polar cap angle will cause the decrease of X-ray luminosity and enhanced spindown rate of SGR J1745-2900. This magnetar is shortly expected to have a maximum spindown rate.