Accretion-disc radius variations in close binaries

Outer radius variations play an important role in the disc structure and evolution. We consider theoretical and observational consequences of such variations in cataclysmic binaries and low-mass X-ray binaries. We find that the action of tidal torques must be important well inside the tidal radius. We also conclude that it is doubtful that the tidal–thermal instability is responsible for the superoutburst/superhump phenomena.     

X 射线照相缺陷定位方法分析与验证

相对于公式法,双标记法解决了焦距和焦点位移测量误差所带来的问题.但此方法在射线检测领域普及程度并不高,其中原因,首先是原理较复杂,针对性研究少,其次是测量精度没有被量化,可信度不高.本文从公式法入手,通过对原理公式的变化分析和线性化分析,明晰了双标记法缺陷深度定位原理,推导了缺陷深度定位公式,利用简化模型,对双标记法的定位精度做了进一步的分析与计算,最后针对具体被检测物,测试验证了双标记法的计算公式和测量精度,用理论和实践证明了方法和精度的可靠性.     

Galaxies at the detection limits of deep X-ray surveys

The great sensitivities of the Chandra X-ray Observatory and XMM-Newton have allowed us to begin to explore the X-ray emission from galaxies at moderate to high redshift. By using the stacking method, we show that we can detect the ensemble emission from normal elliptical, spiral and irregular galaxies out to redshifts approaching unity. The average X-ray luminosity of these galaxy types can then be compared with the results of models of the evolution in the numbers of low-mass and high-mass X-ray binaries and can possibly be used to constrain models of star formation.     

Future X-ray astronomy missions of Japan

Japanese future space programs for high energy astrophysics are presented. The Astro-E2 mission which is the recovery mission of the lost Astro-E has been approved and now scheduled to be put in orbit in early 2005. The design of the whole spacecraft remains the same as that of Astro-E, except for some improvements in the scientific instruments. In spite of the five years of delay, Astro-E2 is still powerful and timely X-ray mission, because of the high energy resolution spectroscopy (FWHM 6 eV in 0.3–10 keV) and high-sensitivity wide-band spectroscopy (0.3–600 keV). The NeXT (New X-ray Telescope) mission, which we propose to have around 2010, succeeds and extends the science which Astro-E2 will open. It will carry five or six sets of X-ray telescopes which utilize super-mirror technology to enable hard X-ray imaging up to 60–80 keV. In mid-2010s, we would participate in the European XEUS mission, which explores the early (z>5) “hot” universe.     

Present status of very high energy gamma ray observations

Recent results from observations of the southern sky objects are summarized. The unpulsed, persistent very high energy (VHE) emission from the gamma ray pulsars, the Crab and PSR1706-44, is discussed. A process of energetic electrons ejection may take place from a variety of other objects such as from X-ray binaries, similarly to the pulsars. Such an effect may be seen also in pair halos around extragalactic VHE gamma ray emitters, the observational study of which is still in a preliminary stage in the southern hemisphere.     

呈正、负压强指数的复合固体推进剂稳态燃烧模型

通过X光电子能谱和扫描电镜对推进剂和过氯酸铵-粘合剂的多层夹心件之熄火样品的观察,研究了在复合推进剂的燃烧中,压强和添加剂CaCO_3对过氯酸铵被熔化粘合剂覆盖的面积分数(γ)和过氯酸铵的凝相反应分数(G)的影响。在作者已提出的“两区模型”的基础上,发展了一个新的“统一模型”(UM)。该“统一模型”是一个进一步考虑了熔化粘合剂的覆盖,在覆盖下存在反向气化和受燃速调节剂(例如CaCO_3)控制的凝相反应的理论模型。为了计及过氯酸铵颗粒尺寸的分布,像PEM模型一样,统计的方法也被引入了本模型。本模型不仅能用来分析初温、过氯酸铵颗粒尺寸及其分布对燃烧特性的影响,而且可以用来解释平台、麦撤和常规的燃烧特性。同时,本模型还能够成为研究包括负压力指数在内之固体复合推进剂的侵蚀燃烧与燃烧不稳定性研究的基础。     

SLX 1746-311 in outburst

We report on RXTE-PCA observations of SLX 1746-311 during a 100 day outburst in April 2003. We present the 3–20 keV PCA energy spectra of the source and study evolution of spectral parameters. The burst spectrum is soft with T_in 1.3 keV at the beginning of the outburst. There is a clear evidence of a hard power law component throughout the outburst. There is also an indication of a broad iron line. The source exhibits three state transitions with considerable change in the hardness ratio at low count rates. We discuss the possible scenario under which this unusual behaviour can be explained.     

Hard X-Ray Modulation Telescope(HXMT) Mission

The HXMT mission concept consists of a slat-collimated hard X-ray detector assembly sensitive in 20～250 keV with a collection area of about 5000 cm2. Based on the reconstruction technique by direct demodulation developed in recent years, HXMT is mainly devoted to performing a hard X-ray all-sky imaging survey with both high sensitivity and high spatial resolution. It can also be used to make pointed observations of X-ray sources to study their spectroscopic and temporal properties in details. The main detector of HXMT consists of 18 individual cylindrical NaI(T1)/CsI(Na) phoswich modules, each with anarea of 283.5 cm2 and a field of view of 5.7°× 1.1° (FWHM). Its spatial resolution and position accuracy are 5′ and 1′ by using the direct demodulation in 1994, and in 2000 its feasibility and technical demonstration study was selected as a project under the Major State Basic Research Program of China. In October 2005, this project entered the full design phase and was listed as a candidate for the first dedicated astronomy satellite around 2010. We are now also considering secondary low energy instruments for this satellite.     

X-ray populations in galaxies

High-resolution Chandra observations have allowed the detection of populations of X-ray sources in galaxies of all morphological types. The X-ray Luminosity Functions (XLFs) of these X-ray source populations have been derived and studied to uncover the drivers for the formation and evolution of binaries in different stellar populations and environments. These XLFs also provide a tool for identifying the nature of the X-ray source population, since different XLFs characterize X-ray sources belonging to young and old stellar populations. Similarly, X-ray colors can be used for identifying different types of X-ray sources. Ultra-Luminous X-ray sources (ULXs, L_X > 10³⁹ ergs s⁻¹) are found to be associated with star-forming stellar populations. The study of the ULX population of the Antennae galaxies points to compact accreting binaries.     

Black hole spectral states and physical connections

The dramatic changes seen in the X-ray spectral and timing properties of accreting black hole candidates (BHCs) provide important clues about the accretion and jet formation processes that occur in these systems. Dividing the different source behaviors into spectral states provides a framework for studying BHCs. To date, there have been three main classification schemes with Luminosity-based, Component-based, or Transition-based criteria. The canonical, Luminosity-based criteria and physical models that are based on this concept do not provide clear explanations for several phenomena, including hysteresis of spectral states and the presence of jets. I discuss the re-definitions of states, focusing on an application of the Component-based states to more than 400 RXTE observations of the recurrent BHC 4U 1630–47. We compare the X-ray properties for the recent 2002–2004 outburst to those of an earlier (1998) outburst, during which radio jets were observed. The results suggest a connection between hysteresis of states and major jet ejections, and it is possible that both of these are related to the evolution of the inner radius of the optically thick accretion disk.