‘Spectro-temporal’ characteristics and disk-jet connection of the outbursting black hole source XTE J1859+226

We re-investigated the ‘spectro-temporal’ behavior of the source XTE J1859+226 in X-rays during its outburst phase in 1999, by analysing the RXTE PCA/HEXTE data in 2–150 keV spectral band. Detailed analysis shows that the source evolves through different spectral states during its entire outburst as indicated by the variation in the spectral and temporal characteristics. Although the evolution pattern of the outburst followed the typical q-shaped profile, we observed an absence of ‘canonical’ soft state and a weak presence of ‘secondary’ emission during the decay phase of the outburst. The broad-band spectra, modeled with high energy cutoff, shows that the fold-energy increases monotonically in the hard and hard-intermediate states followed by a random variation in the soft-intermediate state. We attempted to estimate the mass of the source based on the evolution of Quasi-Periodic Oscillation (QPO) frequencies during rising phase modeled with the propagating oscillatory shock solution, and from the correlation of photon index and QPO frequency. It is also observed that during multiple ejections (observed as radio flares) the QPO frequencies are not present in the power spectra and there is an absence of lag in the soft to hard photons. The disk flux increases along with a decrease in the high energy flux, implying the soft nature of the spectrum. These results are the ‘possible’ indication that the inner part of the disk (i.e., Comptonized corona), which could be responsible for the generation of QPO and for the non-thermal Comptonized component of the spectrum, is disrupted and the matter gets evacuated in the form of jet. We attempted to explain the complex behavior of ‘spectro-temporal’ properties of the source during the entire outburst and the nature of the disk-jet connection before, during and after the ejection events in the context of two different types of accreting flow material, in presence of magnetic field.     

Polarization effects in radiation from compact X-ray sources

The theory of polarization effects in radiation from compact X-ray sources is presented. The following four problems are considered: 1) the polarization of X-rays from the magnetized neutron stars; 2) the polarization of X-rays from the accretion disk around a black hole; 3) the optical polarization from X-ray binaries, and 4) the results of X-ray polarimetric observations.     

Evolution of solar wind structures from 0.72 to 1 AU

Understanding the evolution of solar wind structures in the inner heliosphere as they approach the Earth is important to space weather prediction. From the in situ solar wind plasma and magnetic field measurements of Pioneer Venus Orbiter (PVO) at 0.72 AU (1979–1988), and of Wind/Advanced Composition Explorer (ACE) missions at 1 AU (1995–2004), we identify and characterize two major solar wind structures, stream interaction regions (SIRs) and interplanetary coronal mass ejections (ICMEs). The average percentage of SIRs occurring with shocks increases significantly from 3% to 24% as they evolve from 0.72 to 1 AU. The average occurrence rate, radial extent, and bulk velocity variation of SIRs do not change from 0.72 to 1 AU, while peak pressure and magnetic field strength both decrease with the radial evolution of SIRs. Within the 0.28 AU distance from the orbit of Venus to that of Earth, the average fraction of ICMEs with shocks increases from 49% to 66%, and the typical radial extent of ICMEs expands by about a fraction of 1.4, with peak pressure and magnetic field strength decreasing significantly. The mean occurrence rate and expansion velocity of ICMEs do not change from 0.72 to 1 AU.     

利用普通钻床或铣床加工高精度坐标孔

本文提供了一种用普通钻床加工高精度坐标孔的方法。提出了联合使用量块和一套导向镗孔装置的解决方案。     

含孔有限大各向异性板的应力集中

 利用经典层板理论，将复合材料层板的弹性问题化归为均匀各向异性板求解，采用各向异性体平面弹性理论中的复势方法，以Ｆａｂｅｒ级数和最小二乘边界配置技术为工具，提出了含孔有限大层板应力集中问题的级数解，详细探讨铺层形式、层板大小、椭圆度等诸参数的影响。     

Evolution of X-ray binaries: Achievements and advances

Three recent developments in the field of formation and evolution of neutron stars and black holes in binaries are addressed:

• The finding that there is a class of neutron stars, formed in interacting binaries, that do not receive kick velocities in their birth events. This finding is particularly important for our understanding of the formation – and formation rates – of double neutron stars. It is argued that these low-kick neutron stars, which tend to have low masses, are formed by a different physical mechanism than the neutron stars that receive large kick velocities at birth.

• The occurrence of velocity kicks in the formation events of stellar black holes.

• The nature of the companions of millisecond X-ray pulsars.

基于CCD的叶片气膜孔快速检测技术研究

研制了一套基于CCD的叶片气膜孔快速检测系统,采用机器视觉的方法,配合四轴测量机构,实现在叶片围绕轴线旋转的同时采集气膜孔的图像,然后利用Halcon图像处理算法库实现图像处理,并计算出气膜孔的尺寸参数。通过对某厂的叶片进行了测量实验,实现了对气膜孔轴线方向和直径的测量,弥补了气膜孔无法定性检测的技术空白,具有推广应用价值。     

Three-dimensional global simulation of multiple ICMEs’ interaction and propagation from the Sun to the heliosphere following the 25–28 October 2003 solar events

This study performs simulations of interplanetary coronal mass ejection (ICME) propagation in a realistic three-dimensional (3D) solar wind structure from the Sun to the Earth by using the newly developed hybrid code, HAFv.2+3DMHD. This model combines two simulation codes, Hakamada–Akasofu–Fry code version 2 (HAFv.2) and a fully 3D, time-dependent MHD simulation code. The solar wind structure is simulated out to 0.08 AU (18 Rs) from source surface maps using the HAFv.2 code. The outputs at 0.08 AU are then used to provide inputs for the lower boundary, at that location, of the 3D MHD code to calculate solar wind and its evolution to 1 AU and beyond. A dynamic disturbance, mimicking a particular flare’s energy output, is delivered to this non-uniform structure to model the evolution and interplanetary propagation of ICMEs (including their shocks). We then show the interaction between two ICMEs and the dynamic process during the overtaking of one shock by the other. The results show that both CMEs and heliosphere current sheet/plasma sheet were deformed by interacting with each other.     

冷却孔非均匀排布波纹板隔热屏冷却特性仿真

为了更加合理地分配冷却气体流量，提高纵向波纹板隔热屏结构的气膜冷却效率，提出了非均匀孔排布局波纹板隔热 屏结构，即保持开孔率不变，构建了上游波纹结构气膜孔排布密集、下游波纹结构气膜孔排布稀疏的非均匀结构。在发动机真实 工况下，采用数值仿真的方法研究了非均匀孔排方式对沿程冷却气体流量分配特性和气膜冷却特性的影响规律，揭示了振幅比变 化对波纹板隔热屏冷却效果的影响规律。结果表明：前密后疏型非均匀孔排布局可以改变冷却气体在隔热屏不同位置处的出流 量，从而显著提高隔热屏的气膜冷却效率。在气膜孔孔参数以及开孔率不变时，增大隔热屏上游孔排密度既可以提高隔热屏上游 的冷却效果，又不会明显降低隔热屏下游的冷却效果，使隔热屏整体面平均气膜冷却效率有所提高，相比于均匀孔排结构，前密后 疏孔排布局最高可使隔热屏面平均气膜冷却效率提高12.66%；在相同工况下，当振幅比从0.035增大至0.075时，隔热屏的面平均 气膜冷却效率显著提高，最高可使其面平均气膜冷却效率提高16.32%。     

Delayed outburst of H 1743–322 in 2003 and relation with its other outbursts

The Galactic transient black hole candidate H 1743–322 exhibited a long duration outburst in 2003 after more than two and a half decades of inactivity. The 2003 event was extensively studied in multi-wavelength bands by many groups. The striking feature is that the total energy released is extremely high as compared to that in tens of outbursts which followed. In this paper, we look at this event and study both the spectral and temporal properties of the source using two component advective flow (TCAF) paradigm. We extract accretion flow parameters for each observation from spectral properties of the decay phase and determine the mass of the black hole. We computed the energy released during all the known outbursts since 2003 and showed that on an average, the energy release in an outburst is proportional to the duration of the quiescent state just prior to it, with the exception of the 2004 outburst. A constant rate of supply of matter from the companion cannot explain the energy release in 2004 outburst. However, if the energy release of 2003 is incomplete and the leftover is released in 2004, then the companion’s rate of matter supply can be constant since 1977 till date. We believe that erratic behaviour of viscosity at the accumulation radius $X_p$ of matter as well as location the $X_p$ itself, rather than the random variation of mass transfer rate from the companion, could be responsible for non-uniformity in outburst pattern. We discuss several factors on which the waiting time and duration of the next outburst could depend.