基于Logistic回归模型的Blazar天体的分类

从文献中收集了205个Blazar天体,包括142个BL Lac天体和63个平谱射电类星体(FSRQs).对这些天体的类别与它们的红移、射电5 GHz辐射流量、光学V波段流量、1 keV处X射线流量、X射线光子谱指数进行了相关性和Logistic回归分析.结果表明,对Blazar天体分类产生主要影响的因素是红移、射电5 GHz辐射流量和X射线光子谱指数,综合应用这三个物理量判别Blazar天体的分类的准确率可达到91.2%,得到的分类方程具有良好的预测效果,可以作为Blazar天体分类的一个重要的判据.而光学V波段流量和1 keV处X射线流量不能区分开BL Lac天体和FSRQs,它们与Blazar天体分类没有相关性.本文结果支持将BL Lac天体和FSRQs归为Blazar天体,不同类别的Blazar天体之间能通过一种演化序列相联系. 关键词： Logistic 分类 Blazar天体     

The rms-flux relation of Cyg X-2 in the horizontal branch

We have investigated the relation between the root mean square (rms) variability and the X-ray flux (rms-flux relation) of the Z source Cyg X-2, and as well the energy dependence based on the Rossi X-ray Timing Explorer (RXTE) observations. We currently focus on the horizontal branch (HB), due to the negative correlation in flux of the soft and the hard X-rays. The rms-flux correlation has energy dependence as follows: positive at hard X-rays (above 10 keV) but negative at soft X-rays (below 10 keV). This provides a feature different from the previous one, and may be suggestive of different origins of X-rays below and above 10 keV. Nevertheless, the overall spectrum can be well fitted with a model consisting of a blackbody and Comptonization components, but the fitting results do not reveal any features around 10 keV that could account for such a change in the rms-flux relation.     

The origin of the continuum of Active Galactic Nuclei

Summary The high-energy continuum of active galactic nuclei can be interpreted by nonthermal models in which electron-positron pairs play a crucial role. The produced primary γ-rays interact with softer photons in the inner, high photon density regions of the source. The created pairs are relativistic, and contribute to the emission, especially in the X-ray band. When the photon density is large enough, therefore for large values of the luminosity-to size ratio, the spectrum produced by the reprocessing due to pairs is predicted to have a characteristic spectral index of one. This power law continuum partly impinges on cold matter, possibly in an accretion disk. The resulting Compton reflected radiation contributes to the X-ray emission, and the predicted overall spectrum is in agreement with the observed shape of the high-energy continuum. The proposed model is easily testable: observations in the hard—X-ray band above (30÷50) keV are crucial to discriminate these nonthermal models against thermal ones. Paper presented at the V Cosmic Physics National Conference, S. Miniato, November 27–30, 1990.     

The flux modulation of INTEGRAL

We have analyzed International Gamma-Ray Astrophysics Laboratory (INTEGRAL) data corresponding to observations of the high mass X-ray binary (HMXB) V0332+53 during its huge outburst which occurred in 2004–2005, and found that there is a quasi periodic signal with ultra low frequency of roughly 4−5×10⁻⁵ Hz in the observation. This feature is revealed through a series of consistent analyses of imagings and fittings of the energy spectrum for each science window (SCW), and shows up in the corresponding light curves. The analysis of the power spectrum also provides a hint of a power peak located around 4×10⁻⁵ Hz, after subtracting off the linear trend of the light curve, and shows the consistency with the previous analyses. A similar feature shows up in our analysis of the light curve of Crab in hexagonal dithering mode. Therefore, an instrumental effect on the flux modulation might exist in the INTEGRAL data product of different levels: imaging, spectral fitting and light curve analysis, at least for the observational mode of hexagonal dithering. Such an effect is, to our knowledge, not yet available in the current literature.

     

Broad-band X-ray spectrum of the bright Seyfert galaxy Mkn 509

Summary One of the brightest X-ray Seyfert galaxies, Mkn 509, has been observed with the X-ray satellite EXOSAT. Wide-band ((0.05÷35) keV) spectral information is now available at the same time. Different filters have been rotated in front of the low-energy telescope. The overall spectrum is best fitted by a two-component power law. The intensity and the spectral index of the soft component are in agreement with the extrapotation of the UV spectrum; the high-energy component exhibits a spectral index harder than reported by previous observations and a correspondingly lower intensity. Therefore, at least for this source, the predicted low-energy spectral turnover is a smooth prolungation of the UV spectrum rather than a sharp discontinuity. Paper presented at the 2° Convegno Nazionale di Fisica Cosmica, held at L'Aquila, 29 May – 2 June 1984.     

Afterglow from GRB 070610/Swift J195509.6+261406: An explanation using the fireball model

GRB 070610, which is also named Swift J195509.6+261406, is a peculiar Galactic transient with significant variability on short timescales in both X-ray and optical light curves. One possible explanation is that GRB 070610/Swift J195509.6 + 261406 is a soft gamma-ray repeater (SGR) in our Galaxy. Here, we use the fireball model, which is usually recognized as the standard model of gamma-ray burst (GRB) afterglows, and the energy injection hypothesis to interpret the X-ray and optical afterglow light curves of GRB 070610/Swift J195509.6 + 261406. It is found that the model is generally consistent with observations.

     

Monte Carlo simulation of the dose deposited into GAFCHROMIC® film by X-rays produced by the electron beam of PFMA-3

The electron beam emitted backward by Plasma Focus devices is being investigated as a radiation source for IORT (Intra-Operative Radiation Therapy) applications. A Plasma Focus device is being developed to this aim, to be utilized as an X-ray source. The electron beam is driven to impinge on a 50 μm brass foil, where conversion X-rays are generated. Monte Carlo simulations of the X-ray emission have been conducted with MCNPX, with the purpose of estimating penetration in and dose to human tissue. The electron spectrum had been determined experimentally and is used in the present work as input to the simulations. X-ray emission both from bremsstrahlung and from characteristic lines is predicted. The spectrum is found to be comprised of two components: one peaked at 10 keV and one centred around 50 keV. Doses to film determined from the present simulations are compared to experimental values obtained in a previous work by the authors: the results are found in very good agreement.     

Simulation of muon-induced air showers affecting CMS tracking detectors

We study the propagation of energetic muons produced by ultrahigh energy cosmic rays which could penetrate the cavern of a giant experiment called Compact Muon Solenoid (CMS) at CERN. The present work is based on our previous simulation model proposed in [1]. We have improved this model by (1) eliminating the ambiguity via adding Landau-Pomeranchuk-Migdal effect to the Monte-Carlo code, (2) using different incidence angles of the simulated air showers, (3) defining the actual contents of the CMS cavern concrete. We estimate the energy spectrum of muons produced by air showers of primary protons and photons, which could be detected as a background in the CMS tracking detectors. Our results show that muons produced by air showers within the energy range 10¹⁷–10²⁰ eV injected to the CMS site could penetrate the cavern with cutoff energy 36.5 GeV. The article is published in the original.     

空间相干与入射光子能量对临床类同轴X射线相衬成像影响

在临床实际应用中,X射线源是一个具有有限尺寸的多色光源.基于Fresnel-Kirchhoff衍射理论,考虑空间相干的影响,新的类同轴X射线相衬成像公式被导出.分别代表吸收效应与相位效应的吸收衬度传递函数和相位衬度传递函数从新公式得到.吸收衬度传递函数和相位衬度传递函数的曲线由Matlab给出,不同源半径的最佳成像位置也被计算.理论分析结果如下:1）当光源半径足够大时空间相干效应须被考虑,减小源半径可以增强相位效应|2）源半径与最佳成像位置间有确定关系,并在本文中给出|3）源尺寸效应对相位效应影响不是无限的|4）减小入射X射线光子能量将会显著增强相位效应,但不会对最佳成像位置有影响,因此,上述结论可以被拓展到多色光情况.为了验证理论结果,本文给出了对一个表面破损的光学玻璃微聚焦相衬成像的实验结果.其中一些实验结果与理论分析符合很好,但也有一些实验未达到预期,相关的解释文中也已给出.     

Generation of X-rays due to multiple runaway breakdown inside thunderclouds

Generation of X-rays due to multiple runaway breakdown inside thunderclouds is discussed. The model is based on the recently developed kinetic theory of the runaway breakdown, and detailed theory of the X-rays propagation in the atmosphere from the source to detector, which is determined by the Compton scattering. The model is shown to be in qualitative agreement with observations of the X-ray spectrum. A comparison with the observed electric field distribution and X-ray emission is consistent with the existence of a preconditioning fast charge transfer. Both fast electrons having short lifetime and slow moving ions having long lifetime make a significant input into the charge transfer.     

Comparing potential-driven DBI-inspired non-minimal kinetic coupling(Dinkic) inflation with observational data

In our previous work [1], a new kind of inflation model was proposed, which has the interesting property that its perturbation equation of motion gets a correction of k4, due to the non-linearity of the kinetic term.Nonetheless, the scale-invariance of the power spectrum remains valid, both in large-k and small-k limits. In this paper, we investigate in detail the spectral index, the index running and the tensor/scalar ratio in this model, especially in the potential-driven case, and compare the results with the current PLANCK/BICEP observational data.We also discuss the tensor spectrum in this case, which is expected to be tested by future observations of primordial gravitational waves.     

空间相干与入射光子能量对临床类同轴X射线相衬成像影响

在临床实际应用中,X射线源是一个具有有限尺寸的多色光源.基于Fresnel-Kirchhoff衍射理论,考虑空间相干的影响,新的类同轴X射线相衬成像公式被导出.分别代表吸收效应与相位效应的吸收衬度传递函数和相位衬度传递函数从新公式得到.吸收衬度传递函数和相位衬度传递函数的曲线由Matlab给出,不同源半径的最佳成像位置...     

High Pressure X-Ray Absorption and Diffraction Study of InAs

We have performed X-ray absorption (XAS) and diffraction (XRD) measurements at high pressure on samples of powdered InAs, up to 50 and 80 GPa, respectively. In the lower pressure range, our data are consistent with the following structural sequence: Zincblende M NaCl M Cmcm . The first order transition from the semiconducting Zincblende phase to the metallic NaCl phase is clearly seen by the shift in the absorption onset at the As K-edge and the strong modifications of the extended X-ray absorption fine structure (EXAFS) due to the changes in the local structure from a 4-fold to a 6-fold coordinated environment. XAS shows the high pressure phase to be locally site-ordered. The diffraction data, analized by Rietveld fitting, gives a volume discontinuity of j V/V 0 ～0.18 for the first order transition. There is no apparent volume discontinuity associated to the NaCl M Cmcm transition.     

Three years’ systematic GRB follow-up at the Xinglong Observatory and the optical afterglow observations of GRB 080330

We present a brief overview of follow-up observations of GRB afterglows made by the 0.8-m TNT and other telescopes at the Xinglong observatory during the last three years. Our system, dedicated to the measurement of early-time optical afterglow emission, responded to 50 GRBs from Jan. 2006 to Apr. 2009. Among them, about 50% have been successfully detected. The fastest response time is 76 sec (GRB 061110A and GRB 090426) after the space-borne GRB detector was triggered. The redshift distribution spans the range from z = 0.033 (GRB 060218) to z = 5.6 (GRB 060927). We also report the optical photometric follow-up of GRB 080330, which is an X-ray flash, as an example of our observations.     

Effect of temperature on pulsed laser deposition of ZnO films

ZnO thin films have been deposited on Si(1 1 1) substrates at different substrate temperature by pulsed laser deposition (PLD) of ZnO target in oxygen atmosphere. An Nd:YAG pulsed laser with a wavelength of 1064 nm was used as laser source. The influences of the deposition temperature on the thickness, crystallinity, surface morphology and optical properties of ZnO films were characterized by X-ray diffraction (XRD), scanning electron microscopy (SEM), selected area electron diffraction (SAED), photoluminescence (PL) spectrum and infrared spectrum. The results show that in our experimental conditions, the ZnO thin films deposited at 400 °C have the best surface morphology and crystalline quality. And the PL spectrum with the strongest ultraviolet (UV) peak and blue peak is observed in this condition.     

X射线能量谱间接测量方法

X光机的X射线能量谱在CT图像硬化校正、散射校正和定量CT成像等技术中扮演着重要角色。提出了一种通过由质量衰减系数已知的材料构成的楔型模体的扫描数据来恢复X射线能量谱的方法。经GEANT4模拟数据及实采数据验证,该方法能够较好地恢复X光机的X射线能量谱。通过仿真实验,分析了在几个常用电压下模体材质和厚度对恢复X射线能量谱的影响。     

蒙特卡罗模拟元素特征X射线注量的展宽技术

蒙特卡罗模拟技术可以有效提高核辐射探测分析效率、降低分析成本,在促进X荧光分析技术发展过程中也发挥了重要作用。在应用蒙特卡罗模拟能量色散X荧光分析中,为使蒙特卡罗模拟元素特征X射线注量谱与实验能谱之间的物理差异更小,提出了一种模拟注量展宽算法。首先依据离散统计物理理论,建立了Si-PIN半导体探测器对X射线的响应函数模型,并利用加权非线性最小二乘法拟合得到各系数,再对系数进行归一化处理,得到归一化后的响应函数R(E, E′)。然后利用R(E, E′)对模拟注量进行展宽转换,得到脉冲幅度谱(pulse height spectrum, PHS),使模拟谱更趋近于实验谱,这样就可以通过蒙特卡罗模拟得到与实测能谱一致性较高的模拟能谱。研究中最后利用建立的探测器响应函数模型对Ti, V, Cr, Mn, Fe, Ni, Cu, Zn, As, Sn元素K系全能峰拟合χ2_r值在1.04～1.18范围内,对铜合金样品中六种元素特征X射线模拟注量转换结果与实验值一致性较好,并实现了对多元素混合样品复杂重迭谱的有效模拟和展宽。     

On Braneworld inflation models in light of WMAP7 data

We are interested on studying various inflationary spectrum perturbation parameters in the context of the Randall-Sandrum type 2 Braneworld model. We consider in particular three types of potentials. We apply the slow-roll approximation in the high energy limit to constraint the parameter potentials by confronting our results to recent WMAP7 observations. We show that, for some values of the e-folding number N, the monomial potential provides the best fit results to observations data.     

X-ray spectral signatures of very thick cold matter in the Spectra of seyfert galaxies

Summary Over the last few years, GINGA observations of several bright Seyfert galaxies have revealed the existence of a new flat component in the X-ray spectrum of these objects above 8 keV. This component (the ?high-energy bump?) is probably produced by the reprocessing of the intrinsic emission (through Compton scattering and photoelectric absorption) by a very thick and cold medium in the environment of the central source, such as an accretion disk. An alternative explanation is provided by partial covering and reprocessing by thick clouds, whose existence is supported by the latest results on the broad line region obtained by line reverberation measurements in the optical-ultraviolet band. The presence of iron fluorescent lines at 6.4 keV with an equivalent width ≅ (100÷200) eV in all those galaxies supports both scenarios. The implications of the presence of the high-energy bump on the spectral shape of the intrinsic continuum, the level of the soft X-ray excess and the X-ray background are briefly pointed out. Paper presented at the V Cosmic Physics National Conference, S. Miniato, November 27–30, 1990.