铝基复合材料的脉冲氩弧焊研究

研究了Al_2O_3P/6061Al铝基复合材料在脉冲氩弧焊条件下的可焊性。焊缝金属及热影响区的显微组织观察与分析表明,接头组织致密,无气孔、夹杂和裂纹等缺陷,接头的抗拉强度可达母材强度的80％左右。焊接接头的X射线衍射相结构分析和断口扫描电镜分析的结果表明,接头中含有Al,Al_2O_3,MgAl_2O_4等相,接头拉伸试样断口呈韧性断裂机制。文中还针对这种复合材料在氩弧焊接中存在的问题、以及如何提高接头质量应采取的措施进行了理论探讨。     

A hybrid X-ray imaging spectrometer for NeXT and the next generation X-ray satellite

We propose a new type of wide band X-ray imaging spectrometer as a focal plane detector of the super mirror onboard on future X-ray missions including post Astro-E2. This camera is realized by the hybrid of back illumination CCDs and a back supportless CCD for 0.05–10 keV band, and a Micro Pixel Gas Chamber detecting X-rays at 10–80 keV.     

The optical to X-ray spectrum of the broad-line ultrasoft AGN RE J2248-511

We present a series of monitoring observations of the ultrasoft broad-line Seyfert galaxy RE J2248-511 with XMM-Newton. Previous X-ray observations showed a transition from a very soft state to a harder state five years later. We find that the ultrasoft X-ray excess has re-emerged, yet there is no change in the hard power-law. Reflection models with a reflection fraction of 15, and Comptonisation models with two components of different temperatures and optical depths (kT₁ = 83 keV, T₁ = 30 eV, τ₁ = 0.8; KT₂ = 3.5 keV, T₂ = 60 eV, τ₂ = 2.8) can be fit to the spectrum, but cannot be constrained. The best representation of the spectrum is a model consisting of two blackbodies (kT₁ = 0.09 ± 0.01 keV, kT₂ = 0.21 ± 0.03 keV) plus a power-law (Γ = 1.8 ± 0.08). We also present simultaneous optical and infrared data showing that the optical spectral slope also changes dramatically on timescales of years. If the optical to X-ray flux comes primarily from a Comptonised accretion disk we obtain estimates for the black hole mass , accretion rate and inclination cos(i)  0.8 of the disk.     

Study of the luminosity-dependent cyclotron resonance energies of the binary X-ray pulsar 4U 0115+63 with RXTE

We report on the luminosity dependent change of the cyclotron resonance energy obtained from a transient X-ray pulsar, 4U 0115+63. Using RXTE data observed on 1999 March, we found that the fundamental resonance energy stayed constant (11 keV) when the source luminosity was above 5 × 10³⁷ erg s⁻¹. As the luminosity decreased below 5 × 10³⁷ erg s⁻¹, the fundamental resonance energy gradually increased up to 16 keV at 0.16 × 10³⁷ erg s⁻¹. The luminosity dependence of the resonance energy can be understood by the change of the accretion column height.     

Hard X-ray emission from the recurrent transient A0535+26 during its 1980 high-intensity outburst

The transient X-ray pulsar A0535+26 was observed on October 4, 1980 during a high level intensity outburst with a balloon borne hard X-ray detector. High statistical quality source spectra were determined up to 100 keV. Both blackbody and Wien laws fit well the data. Pulse phase spectroscopy shows variation of temperature index between 7.5 and 8.5 keV in the off source spectra and between 7.4 and 10.5 keV in the off pulse spectra. The time averaged luminosity above 30 keV is 8×10³⁶ erg/s.     

Optical pre-nova identification for the X-ray Nova GRO J0422+32 (Nova Persei, 1992)

The X-ray Nova GRO J0422+32 in its low brightness has been identified with a B 21 ^m , R20 ^m star on Palomar Sky Survey glass copies. The scans obtained with an automatical microdensitometer along with our special PC program were used. The resulting outburst amplitude 8 ^m is one of similarity features for the class of the low mass X-ray Novae, black hole candidates.     

康普顿散射对X射线热激波破坏效应的影响

本文应用ＧＲＡＹ三相物态方程及Ｌａｇｒａｎｇｅ数值模拟方法，计算并讨论了康普顿散射对Ｘ射线热激波及其破坏效应的影响。计算结果表明，对较硬的Ｘ射线谱（１５ｋｅＶＰｌａｎｃｋ谱），康普顿散造成量沉积与热击波峰压明显下降，在ＬＹ－１２铝中，能量沉积的相对差△Ｅ（ｘ）／Ｅ（ｘ）可达９％－２２％，热击波峰压的相对差△ｐｍ（ｘ）／ｐｍ（ｘ）约为１２％。     

The revised eccentric binary model for X Persei (4U 0352 + 30)

The eccentric binary model for X Persei is discussed with a view to most recent determination of mass, radius and mass loss rate. The existence of such a system depends critically on the value of viscosity in the outer layers of the star and, in the case where viscosity is induced by shear turbolence, on the axial rotational velocity. The parameters of the binary system are derived in the most favourable case.     

Review on latest progress on supergiant fast X-ray transients and future direction

In the recent years, the discovery of a new class of Galactic transients with fast and bright flaring X-ray activity, the supergiant fast X-ray transients, has completely changed our view and comprehension of massive X-ray binaries. These objects display X-ray outbursts which are difficult to be explained in the framework of standard theories for the accretion of matter onto compact objects, and could represent a dominant population of X-ray binaries. I will review their main observational properties (neutron star magnetic field, orbital and spin period, long term behavior, duty cycle, quiescence and outburst emission), which pose serious problems to the main mechanisms recently proposed to explain their X-ray behavior. I will discuss both present results and future perspectives with the next generation of X-ray telescopes.     

On the motions of RHESSI flare footpoints

The footpoint motions of flare hard X-ray (HXR) sources are directly related to the reconnection scenario of a solar flare. In this work, we tried to extract the information of footpoint motions for a number of flares observed with RHESSI. We found that the RHESSI flare results of the footpoint motions strongly support the classification proposed from the observations of YOHKOH/HXT. Furthermore, it is found that a flare can consist of two types of footpoint motions. We discussed the connections of the footpoint motions with the two-dimensional reconnection models.