微型X射线管出射谱特征研究及Be窗厚度确定

微型X射线管已广泛应用于现场元素分析、放射性医疗等领域,对于微型X射线管铍窗,普遍认为除保证管内真空外,应越薄越好。采用蒙特卡洛方法,模拟了从50～500 μm范围内共13个Be窗厚度的微型X射线管出射X射线谱。按照在应用中的作用,将出射X射线划分为不同能量段进行分析。通过分析谱线特征,发现Be窗厚度应依据其应用要求合理选择。因此,提出了K系特征X射线与轫致辐射强度的比值和低能射线与激发射线计数比值等参量作为评价Be窗厚度最优化的判断依据。除上述评判指标外,铍窗的厚度最优化选择还应考虑Be窗对不同能量X射线的屏蔽效果。依据模拟结果分析,原位(现场)X射线能量色散荧光分析应用中,Be窗厚度约250 μm的微型X射线管最为合适。与50 μm铍窗厚度出射射线相比,71.66%低能原级X射线被屏蔽,5~50 keV能量原级X射线仅有21.31%被屏蔽,低能射线强度占总X射线比值小于10%,且K系X射线占激发射线的比例仍保持较高的水平。因此,采用250 μm铍窗厚度的微型X射线管作为能量色散激发源,能保证探测器探测的有效信号比值较高,低能X射线对探测器的能量分辨率的影响最小,而且能量色散分析谱线的散射本底相对强度处于较低的水平,从而保证元素分析结果精准度。对于放射性治疗的应用中,则铍窗厚度越薄越好,此时,低能X射线具有较高的通量,能保证辐射剂量在治疗组织中剂量的集中。     

Effect of Opacity on the Solar Spectral Line of C I 165.7 nm by Escape Factor Treatment

In this article, we report that by using the intensity ratio of the (2-2) to (1-2) component of CI emission lines at about 165.7 nm, we determined the optical depth at the line center of the (2-2) component of CI emission lines by escape factor treatment. The optical depth at the line center of the (2-2) component is calculated to be 0.9998, which is a more reasonable value of solar spectral lines than the value that has been reported. The variation of the optical depth at the line center for different positions from the solar limb is discussed. Using the measured abundance of carbon and the results of ionization balance calculations, we estimate the electron density in the CI emitting region. The density of hydrogen is estimated in the CI emitting region by this method, and is testified to be a better value than the value that has been reported. This discussion will be significant in the analysis of opacity on the solar ultraviolet (UV) or extreme-ultraviolet (EUV) spectrum.     

Density functional studies on lanthanide (III) texaphyrins (Ln-Tex2+, Ln = La,Gd, Lu): structure,stability and electronic excitation spectrum

Density functional calculations have been performed to study the molecular structure and chemical properties of selected lanthanide(III) texaphyrins (Ln-Tex²⁺, Ln = La, Gd, Lu). The lanthanide element is found to reside above the mean N₅ texaphyrin plane, and the larger the cation, the greater the observed out-of-plane displacement. It is concluded that the lanthanide cation is tightly bound to the macrocyclic skeleton, yielding a stable structure. However, the chemical properties of Ln-Tex²⁺ are found to be only slightly affected by the substitution of the lanthanide element. A low-energy LUMO is found for the Ln-Tex²⁺ (Ln = La, Gd, Lu), which are therefore easily reduced in an electron-rich environment. Two characteristic bands are obtained in the calculated electronic excitation spectrum (a high-energy band at 454–462 nm and a low-energy band at 681–686 nm). The intensity of the high-energy band is much larger than that of the low-energy one, yielding a rather unique spectral feature.     

Development of online quasimonochromatic X-ray backlighter for high energy density physics studies

Monochromatic X-ray backlighting has been employed with great success in various laser plasma experiments including inertial confinement fusion (ICF) research. However, implementation of a monochromatic backlighting system typically requires extremely high quality spherically bent crystals which are difficult to manufacture and are also expensive. In this paper, we present a quasimonochromatic X-ray backlighting system using flat thallium acid pthalate (TAP) crystal. The detailed characterization of the system is discussed. The X-ray backlighter spectral range is caliberated using Cu spectrum in the spectral range 7–9 Å (1.38–1.77 keV). Gold plasma produces continuous X-ray spectrum (M band) in this range. The spectral, spatial and temporal resolutions of the system measured are 30 mÅ, 50 μm and 1.5 ns respectively. The spectral width of the X-ray pulse is 2 Å (ΔE = 0.39 keV).     

The investigation of the Neupert effect in two solar flares

The Neupert effect suggests a flare model in which the nonthermal emissions are produced by energetic electrons which heat lower corona and chromosphere to produce the thermal emissions. Based on this concept, we investigate the Neupert effect to test the correlation between the hard X-ray spectral index and the time rate of the UV flare area at 1600 or 171 Å. Using the TRACE and RHESSI observations, we explore these quantities for two solar flares, one on March 14, 2002 and the other on November 1, 2003. The negative dependence between the spectral index and the time rate of the UV flare area is found, especially during the hard X-ray sub-peaks. This finding indicates that the electron-beam-driven heating plays a prominent role in the UV emission of these two flares.     

西藏地面太阳总辐射与紫外线的观测

地面太阳光谱记录了太阳光经历大气层的烙印与信息,为大气环境、生态保护等研究提供实地依据。西藏高原空气稀薄,地面太阳辐射超强,观测西藏地面太阳光谱为太阳能利用提供实地数据。文章较系统地报道了西藏地面太阳光谱的实地观测结果,为相关高原科学研究提供高精度数据。利用RAMSES光谱仪、CMP6太阳总辐射仪和NILU-UV太阳紫外辐射仪对西藏不同地区、不同季节太阳光谱、太阳总辐射和太阳紫外线进行了全方位的实地观测研究。观测研究了高海拔的西藏拉萨和那曲以及低海拔的北京和成都的光谱特征;研究了拉萨二分二至当地正午（北京时间13:55时）太阳光谱观测结果;对西藏地面光谱与AM1.5和AM0标准光谱进行了对比研究。观测研究了西藏拉萨和那曲太阳总辐射、太阳紫外线强度特征。研究发现拉萨夏季可见和红外区光谱光强度甚至超过AM0光谱相应波长的强度,即：拉萨地面可见光和红外光强度偶尔超过大气层顶部的相应波长光强,是由部分云的反射增量所致;拉萨光谱谱峰出现在波长476.6 nm左右,在2017年的夏至观测到的最大值为2.331 W·m-2·nm-1。然而,对太阳紫外线（280～400 nm）光谱的观测发现地面太阳紫外区的光谱强度总是明显低于AM0光谱相应区光强,表明短波的紫外光被大气臭氧有效吸收。虽然拉萨海拔3 680 m,但通过对拉萨当地正午太阳紫外光谱分析发现拉萨地面波长小于300 nm的太阳紫外光谱强度几乎为零,表明波长小于300 nm的太阳紫外线被大气层吸收,没有到达地面。同时,研究了西藏高海拔太阳光谱与北京、成都低海拔太阳光谱特征,揭示了各地大气成分、含量等诸多信息。报道了2010年7月-2013年12月期间西藏太阳总辐射的观测结果;结果显示拉萨当日太阳总辐射最大值中约18%超过了太阳常数（1 367 W·m-2）。观测发现拉萨太阳总辐射瞬时最大值达到了1 756.09 W·m-2（2011年6月24日）。报道了2008年7月-2013年12月期间西藏太阳紫外线的观测结果;结果显示拉萨和那曲UVA日最大值平均值约为67 W·m-2,UVB日最大值平均值约为5.1 W·m-2;拉萨和那曲当日太阳紫外线A和紫外线B最大值变化趋势保持了很好的一致性,在5年多的观测期间紫外线强度没有出现明显的增强或减弱趋势。     

真空、低能离子注入后HeLa细胞的吸收光谱研究

在选用了石蜡油作为细胞耐受真空的保护剂基础上,分别采集了人宫颈癌细胞(HeLa细胞)经真空和不同剂量低能离子注入后的紫外吸收光谱.实验结果显示:HeLa细胞在202及260 nm附近均有特征性的吸收峰.数据的进一步分析发现:(1)HeLa细胞经真空处理后的紫外吸光值随着真空时间的延长而增加,且真空对细胞紫外吸收光谱的影响大于单纯的石蜡油浸泡影响;(2)真空对于HeLa细胞紫外吸光值的影响远低于低能离子注入的影响;(3)HeLa细胞在注入不同剂量的低能N+后,紫外吸光值会随着注入剂量的增大而增加.在上述分析的基础上,本文又探讨了低能N+束注入对肿瘤细胞的结构、各成分的组成比例及分子排列的影响,该研究为深入探索低能离子注入生物样品的作用机理奠定了基础.     

High resolution absorption and magnetic circular dichroism of spin-forbidden ligand field transitions in Cs3CoBr5

The axial absorption spectrum of Cs₃CoBr₅ has been recorded from 3100 to 6500 Å at 4·2 K with a spectral bandpass of 0·1 Å and the magnetic circular dichroism spectrum at 4·2 K and 47·5 kG over the same wavelength range with a spectral bandpass of 1 Å. The electronic origins of the spinorbit and tetragonal field components of most of the doublet ligand field states are definitively located and assigned. In a number of instances it has also proved possible to determine whether the doublet gains its intensity from the 3/2 U′ or 5/2 U′ spin-orbit component of ⁴ T ₁, and arguments are also presented to show that the higher energy doublets derive the greater part of their intensity from the lowest ⁴ T ₁ charge transfer state and not the ⁴ T ₁(P) ligand field state. The vibronic sidebands accompanying the doublet transitions are also assigned to internal modes of CoBr₄ ^2- and to lattice modes. In a number of the transitions non-totally symmetric modes are excited with greater intensity than totally symmetric.     

Photo- and Thermobleaching of Luminescence Centers in Synthetic Opals

It has been found that on exposure of specimens of synthetic opal to UV radiation, luminescence is excited in them (337 nm) that has spectral maxima at 400 and 500 nm. Its duration at half-height of a pulse is 9 nsec, and there is a weak slow component with τ ∼ 1 μsec. The spectrum and intensity of the luminescence depend on the duration of irradiation and temperature. The luminescence bands revealed relate to two individual luminescence centers, namely: the shortwave one, caused by the luminescence centers formed in the bulk of the opal, and the longwave one, due to those formed on the opal surface. __________ Translated from Zhurnal Prikladnoi Spektroskopii, Vol. 72, No. 5, pp. 622–626, September–October, 2005.     

Spectroscopy of composite scintillators

The spectral and temporal characteristics of X-ray luminescence of composites consisting of microparticles of “heavy” components (oxides, fluorides, sulfates) and an organic polymer binder containing optically active impurities have been investigated. It has been found that, in the case of pulsed X-ray excitation of the composites with a photon energy of 130–150 keV, the fast component (τ < 10 ns) of the luminescence arises whether or not the “heavy” component of the composite is doped with an optically active impurity. A mechanism has been proposed for the formation of the fast component of the luminescence: electrons and low-energy X-ray photons generated during the interaction of high-energy X-ray photons with the “heavy” component of the composite are effectively absorbed by the polymer binder and, thus, induce its luminescence. It has been shown that, in order to produce a composite-based fast scintillator with a high light yield, it is necessary to use a binder prepared from an organic material with a short scintillation decay time and another component prepared from a compound whose composition includes an element of a large atomic number Z.     

A black hole spectral signature

An accreting black hole is, by definition, characterized by the drain. Namely, the matter falls into a black hole much the same way as water disappears down a drain — matter goes in and nothing comes out. As this can only happen in a black hole, it provides a way to see “a black hole”, an unique observational signature. The accretion proceeds almost in a free-fall manner close to the black hole horizon, where the strong gravitational field dominates the pressure forces. In this paper we present analytical calculations and Monte-Carlo simulations of the specific features of X-ray spectra formed as a result of upscattering of the soft (disk) photons in the converging inflow (CI) into the black hole. The full relativistic treatment has been implemented to reproduce these spectra. We show that spectra in the soft state of black hole systems (BHS) can be described as the sum of a thermal (disk) component and the convolution of some fraction of this component with the CI upscattering spread (Greens) function. The latter boosted photon component is seen as an extended power-law at energies much higher than the characteristic energy of the soft photons. We demonstrate the stability of the power spectral index over a wide range of the plasma temperature 0 – 10 keV and mass accretion rates (higher than 2 in Eddington units). We also demonstrate that the sharp high energy cutoff occurs at energies of 200–400 keV which are related to the average energy of electrons m_ec² impinging upon the event horizon. The spectrum is practically identical to the standard thermal Comptonization spectrum when the CI plasma temperature is getting of order of 50 keV (the typical ones for the hard state of BHS). In this case one can see the effect of the bulk motion only at high energies where there is an excess in the CI spectrum with respect to the pure thermal one. Furthermore we demonstrate that the change of spectral shapes from the soft X-ray state to the hard X-ray state is clearly to be related with the temperature of the bulk flow. In other words the effect of the bulk Comptonization compared to the thermal one is getting stronger when the plasma temperature drops below 10 keV. We clearly demonstrate that these spectra emerging from the converging inflow are a inevitable stamp of the BHS where the strong gravitational field dominates the pressure forces.     

Electronic spectra of potassium bromide containing thallium II. Emission spectrum excited at 2537 Å

The emission spectrum of KBr: Tl⁺ excited at 2537 Å has been measured in the temperature range 15–296°K. At low temperatures the spectrum consists of a prominent band at 4.01 eV, a much smaller band at 3.40 eV and a very small band at 3.15 eV. The last does not appear to change much with temperature and so could not be measured accurately. The temperature-dependence of the two main bands is complex. Between 60 and 100°K the low-energy band increases sharply in intensity, while the high-energy band decreases correspondingly. Above 110°K the situation reverses and the low-energy band decreases in intensity while the high-energy band grows. Both bands closely approximate symmetric Gaussians. The temperature-dependence of the intensity of these two bands is well-explained qualitatively by the existence of two kinds of minima on the adiabatic potential energy surface for the A state. However, predictions of the temperature-dependence of the two emission bands based on calculated adiabatic potential energy surfaces are not in quantitative agreement with the experimental results. Possible reasons for this are our lack of knowledge of precise values for the parameters which enter into the theory, namely the spin-orbit coupling constant, the exchange integral, and the electron lattice coupling constant. The possible role of the ³A_1u state in emission is discussed briefly.     

Analysis of the Opacity of Magnesium XII 0.842 nm Doublet in the Solar Coronal X-ray Spectrum

Using the observed intensity ratio of the magnesium XII 0.842 nm doublet in the solar coronal X-ray spectrum, we investigate the opacity of the (1/2–3/2) component of the magnesium XII doublet. The escape factor and the opacity of the (1/2–3/2) component of the magnesium XII 0.842 nm doublet are discussed. Results show that the opacity has great effect on the (1/2–3/2) component of the magnesium XII 0.842 nm doublet. While using the abundance of magnesium and the results of ionization balance, we calculate the variation of electron density as a function of observed intensity ratio.     

Dual fluorescence of <Emphasis Type="Italic">N</Emphasis>-pyrrolobenzonitrile in extended polyvinyl alcohol films

The possibility of radically changing the conditions for charge transfer (CT) photoreaction in N-pyrrolobenzonitrile molecules in polymer matrices of polyvinyl alcohol (PVA) under their extension has been demonstrated. The fluorescence spectrum of N-pyrrolobenzonitrile in PVA has two characteristic bands in the UV and visible spectral ranges, which are indicative of the CT reaction that occurs in the excited state. Extension significantly reduces the intensity of the UV band, the contribution of which in unstrained samples is comparable with the violet fluorescence intensity. Even a single extension of PVA films significantly reduces the intensity of the UV band, while a sixfold extension dramatically enhances this effect. In the latter case, the fluorescence spectrum contains a strong CT band whose relative intensity exceeds that for highly polar aprotic solvent acetonitrile by a factor of five. The data obtained indicate that, using extension, one can change the main intermolecular factors affecting the CT rate in PVA samples.     

Narrow band X-ray emission in the water-window spectral region from a laser heated gold copper mix-<Emphasis Type="Italic">Z</Emphasis> plasma

A laser plasma X-ray source of narrow spectral range in the water-window region, is reported using a 50–50 (atomic fraction) mixture of gold-copper mix-Z planar target. Plasma was produced using the second harmonic beam of an Nd:glass laser focused to an intensity ～10¹³ W/cm² on the target. The spectrum of the plasma radiation transmitted through a free-standing 0.4 μm aluminium/0.9 μm vanadium X-ray filter foil was measured to lie in the narrow-band of 24–26 Å. This provides a debris-free X-ray dose of 2–3 mJ/sr which can be used for single shot X-ray imaging of live biological samples.     

基于多角度偏振差值曲线的目标识别初探

多角度偏振遥感在目标识别和地物观测中具有广阔的应用前景.从目标地物的偏振探测机理出发,讨论了它们偏振反射光谱的空间特征,以及由反射光的垂直振动分量和平行振动分量构成的偏振差值曲线的变化规律.结果显示:反射光的垂直振动分量与平行振动分量之差R⊥//随着折射率的变化而不同,且均在入射角80°附近达到最大;随着折射率的增加,...     

Time-resolved X-ray diffraction study of the transition of an amorphous TiCu alloy to the crystalline state

The transition of the TiCu alloy from an amorphous state to the crystalline state has been studied by time-resolved X-ray diffraction. An analysis of the diffraction pattern has shown that the crystallization of the amorphous TiCu alloy upon heating occurs for a short time (no longer than 0.5 s). A sharp transition is observed at the instant of crystallization, at which the intensity of the total diffraction pattern background decreases and diffraction lines of the crystalline phase γ-TiCu arise. No intermediate crystalline phases are observed. The change in the alloy structure is accompanied by the exothermic thermal effect. The kinetics of the change in the total intensity of the diffraction spectrum in the period preceding the crystallization is nonmonotonic. Ten seconds before the occurrence of diffraction lines of the γ-TiCu phase at 300°C, the integrated spectral intensity decreases. The effect observed is related to the relaxation processes in the amorphous state and the onset of formation of long-range structural order.     

Photoinduced darkening, crystallization and reversible emission in ZnTe thin films

Laser-induced darkening and crystallization of ZnTe-based thin films is reported. ZnTe thin films of 1500-nm thickness were deposited on bare and Zn buffer layered borosilicate glass substrates. The as-deposited films were subjected to laser irradiation at 532 nm. The as-deposited films were amorphous but transformed to the crystalline state under influence of the laser treatment. The X-ray diffraction patterns revealed that the ZnTe crystallized in the zinc blende structure. In addition, presence of peaks from Te was observed, signifying the dissociation of ZnTe. The spectral transmission of the films decreased by more than 15 % under the influence of the laser irradiation and this was accompanied by a red shift in the band gap. These results clearly point to the occurrence of laser-induced darkening and crystallization of the films. To understand the mechanisms of darkening and crystallization, all the films were annealed at 500 °C for 60 min. Similar to the laser-irradiated samples, the thermally annealed films showed an amorphous–crystalline transition, presence of Te in the X-ray diffraction patterns as well as a large decrease in spectral transmission (>70 %). Photoinduced emission analysis carried out as a function of laser intensities indicated a strong red shift of about 51 meV in emission energy with increase in laser intensity due to the photodarkening. The peak position of the emission spectrum can be tuned by increasing the laser intensity and is completely reversible with decrease in laser intensity. It is proposed that laser-induced darkening occurs due to the dissociation of ZnTe into ZnTe and Te and that crystallization is a consequence of laser annealing.     

Chandra observations of the H2O megamaser galaxy Mrk1210

We present the first Chandra X-ray observations of the H₂O megamaser galaxy Mrk1210 (UGC4203), a Seyfert 2 galaxy at an approximate distance of D ～ 57.6 Mpc. The Chandra X-ray image, with by far the highest angular resolution (～1″), displays an unresolved compact core toward the nuclear region of Mrk1210. Comparisons with the previous X-ray observations in the nuclear emission and the spectral shape indicate a fairly stable phase between 2001 (BeppoSAX and XMM-Newton) and 2004 (Chandra) after a dramatic variation since 1995 (ASCA). The best-fit model of Chandra X-ray spectrum consists of two components. The soft scattered component can be best fitted by a moderately absorbed power-law model adding a spectral line at ～0.9 keV (possibly a Ne-Kα fluorescent line), while the hard nuclear component can be well reproduced by a heavily absorbed power-law model (N _H ～ 2×10²³ cm^?2) with an additional line at ～6.19 keV (close to the Fe-Kα fluorescent line). The derived absorption-corrected X-ray luminosity implies that the dramatic variation of spectral properties is caused by significant changes of the absorbing column density along the line-of-sight, while the intrinsic nuclear X-ray luminosity remains stable. In this case, the absorbers should be anisotropic and its size can be constrained to be less than 0.0013 pc. In addition, we also estimate the mass of central engine, the disk radius and the accretion rate of the accretion disk to be 10^7.12±0.31 M _⊙, ～1 pc and 0.006, respectively.

     

The dependence of muon intensity on the geomagnetic latitude

The vertical momentum spectrum of cosmic-ray muons has been determined by a counter controlled neon-hodoscope in the spectral region (0.2–3) Bev/c at geomagnetic latitude 12 °N. The observed spectrum agrees satisfactorily with the calculated spectrum of Olbert for muon momentum above 1.8 Bev/c. Below about 1.8 Bev/c, the measured spectrum exceeds slightly the theoretical spectrum of Olbert, calculated for the same geomagnetic latitude. The measured spectrum agrees with the experimental spectrum of Allkofer at 9 °N, but is somewhat below the spectrum obtained by Hayman in the low momentum region at 57.5 °N. This shows that there exists a latitude dependence of the low momentum muon spectrum. The estimated integral intensity of muon of momentum ≧320 Mev/c is found to be 7.3×10^?3 cm^?2 sec^?1 str^?1 which agrees with the value of other investigators^1–9.