Application of a relativistic accretion disc model to X-ray spectra of LMC X-1 and GRO J1655-40

We present a general relativistic accretion disc model and its application to the soft-state X-ray spectra of black hole binaries. The model assumes a flat, optically thick disc around a rotating Kerr black hole. The disc locally radiates away the dissipated energy as a blackbody. Special and general relativistic effects influencing photons emitted by the disc are taken into account. The emerging spectrum, as seen by a distant observer, is parametrized by the black hole mass and spin, the accretion rate, the disc inclination angle and the inner disc radius.
We fit the ASCA soft-state X-ray spectra of LMC X-1 and GRO J1655-40 by this model. We find that, having additional limits on the black hole mass and inclination angle from optical/UV observations, we can constrain the black hole spin from X-ray data. In LMC X-1 the constraint is weak, and we can only rule out the maximally rotating black hole. In GRO J1655-40 we can limit the spin much better, and we find 0.68 a 0.88 . Accretion discs in both sources are radiation-pressure dominated. We do not find Compton reflection features in the spectra of any of these objects.     

On the presence of silicon and carbon in the pre-maximum spectrum of the Type Ia SN 1990N

The spectrum of the normal Type Ia SN 1990N observed very early on (14 days before B maximum) was analysed by Fisher et al., who showed that the large width and the unusual profile of the strong line near 6000 Å can be reproduced if the line is assumed to be due to C  ii 6578, 6583 Å and if carbon is located in a high-velocity shell. This line is one of the characterizing features of SNe Ia, and is usually thought to be due to Si  ii . A Monte Carlo spectrum synthesis code is used to investigate this suggestion further. The result is that if a standard explosion model is used, the mass enclosed in the shell at the required high velocity (25 000–35 000 km s⁻¹) is too small to give rise to a strong C  ii line. At the same time, removing silicon has a negative effect on the synthetic spectrum at other wavelengths, and removing carbon from the lower velocity regions near the photosphere makes it difficult to reproduce two weak lines which are naturally explained as C  ii , one of them being the line which Fisher et al. suggested is responsible for the strong 6000-Å feature. However, synthetic spectra confirm that although Si  ii can reproduce most of the observed 6000-Å line, the red wing of the line extends too far to be compatible with a Si  ii origin, and that the flat bottom of the line is also not easy to reproduce. The best fit is obtained for a normal SN Ia abundance mix at velocities near the photosphere (15 500–19 000 km s⁻¹) and an outer carbon–silicon shell beyond 20 000 km s⁻¹. This suggests that mixing is not complete in the outer ejecta of an SN Ia. Observations at even earlier epochs might reveal to what extent a carbon shell is unmixed.     

Spectroscopic observations of SN1987a in the LMC

This paper describes the results of optical spectroscopy of SN1987a carried out at Mt John University Observatory on a regular basis since 1987 February 25. Typical spectra are presented in an evolutionary sequence, and velocities of Balmer and selected metallic lines are measured in either emission or absorption. The velocities are interpreted together with the results of photoelectric photometry. The Barnes-Evans relationship has been applied to the photometry to give an angular diameter of the photosphere. The expansion velocity of the photosphere is initially about 3700 km s^-1 which is similar to the asymptotic value from weaker absorption lines such as the MgIb line. After 40 days the photosphere appears to expand more slowly and it reaches a maximum size of about 145 A.U. after about 100 days before receding inwards. The photometry and spectroscopy together result in a distance modulus of 18.3 ± 0.2.     

The bolometric light curve of SN 1993J and the nature of its progenitor

We have constructed the bolometric light curve of SN 1993J based on UBVRI(JHK) photometric data obtained from various sources and assumingA _V = 0 and a distance modulus of 27.6. Effective temperatures and photosphere radius at various times have been obtained from detailed blackbody fits. The bolometric light curve shows two maxima. The short rise time to the second maximum, and the luminosities at the minimum and the second maximum are used to constrain the properties of the progenitor star. The total mass of the hydrogen envelope M_H, in the star is found to be ≲ 0.2 M_⊙ at the time of explosion, and the explosion ejected about 0.05 M_⊙ of Ni⁵⁶. Thin hydrogen envelope combined with a sufficient presupernova luminosity suggest that the exploding star was in a binary with a probable period range of 5yr ≤P _orb ≤ 11yr.     

软件系统开发中的组件框架技术研究、设计和应用

本文论述了组件技术的发展现状,组件框架的体系结构、组件框架的设计、开发及其选择和应用等问题。     

基于J2EE的分布式网络地理信息服务研究

从目前Web领域的发展现状出发,介绍了Web服务和J2EE架构的定义和特点,介绍了基于J2EE架构的Web应用的多层体系结构模式,并在此架构基础上对如何使用现行的Web服务技术开发Web应用进行了研究。最后给出了分布式网络地理信息服务的具体实现方法。     

基于交通基础地理信息的网络发布研究与实现

近年来随着WebGIS技术的日趋成熟,采用WebGIS技术管理空间数据并进行网络发布,供用户快速查询与使用,实现空间信息的网络共享,为空间数据的充分利用和可视化表达提供了一种有效的解决方案。本文以北京市交通地理信息系统开发为例,探讨了交通基础地理信息的网络发布平台构架设计与实现过程,并针对系统关键技术的原理及实现进行了详细阐述,构建了以J2EE为核心,基于ArcIMS的空间信息服务框架体系,是WebGIS技术在交通领域的集成应用。     

Braking PSR J1734-3333 with a possible fall-back disk

The very small braking index of PSR J1734-3333, n = 0.9 ± 0.2, chal- lenges the current theories of braking mechanisms in pulsars. We present a possible interpretation that this pulsar is surrounded by a fall-hack disk and braked by it. A modified braking torque is proposed based on the competition between the magnetic energy density of the pulsar and the kinetic energy density of the fall-back disk. With this torque, a self-similar disk can fit all the observed parameters of PSR J1734-3333 with natural initial values of parameters. In this regime, the star will evolve to the re- gion having anomalous X-ray pulsars and soft gamma repeaters in the P -/5 diagram in about 20 000 years and stay there for a very long time. The mass of the disk around PSR J1734-3333 in our model is about 10M similar to the observed mass of the disk around AXP 4U 0142＋61.     

云南个旧云掌寨铁矿控矿因素

云掌寨铁矿区地质条件复杂,控矿因素较多,通过分析认为受“层、相、位”控制,地层初始富集,构造及岩浆活动提供通道及热源,热液驱动作用下在构造有利部位成矿.     

基于J2ME的PDA GIS开发

PDA是移动GIS的重要载体,现在的GIS多是针对微机或工作站,不适用于硬件条件较低的PDA平台。基于J2ME技术在PDA平台上开发GIS,探讨基于PDA的GIS软件开发具体技术,介绍笔者在PDA中实现的一个地理信息系统软件。