EXOSAT and EINSTEIN High Resolution Images of the Small Magellanic Cloud

In order to obtain optical identifications and further information about the X-ray emission of sources discovered in the EINSTEIN IPC survey of the Small Magellanic Cloud (SMC), we have used the EXOSAT CMA and EINSTEIN HRI at selected positions. These observations have so far resulted in several identifications (including 4 stellar objects with m_v 14 to 21 and a Seyfert galaxy), and the discovery of two new X-ray sources. Medium energy X-rays (2–6 keV) have been detected from the brightest SNR in the SMC, 1E0102.2-7219. We present here an initial report of these results.     

A dissection of 30 Doradus and a discussion of other Magellanic Cloud OB associations

I Present the results of ground-based and Hubble Space Telescope photometry and spectroscopy of the stars in the central region (roughly 7×7 arcmin) of 30 Doradus in the Large Magellanic Cloud (LMC). Using photometric data for over 2400 stars (complete toV18 mag), and spectroscopic observations of over 150 stars in the region, the best estimate of the initial mass function (IMF) yields a slope of =–1.5±0.2 for masses > 12M, where the Salpeter slope is =–1.35. I compare these results to other measurements of the IMF for OB associations in the Magellanic Clouds.     

The diffuse soft X-ray sky

The current status of the investigation of the soft X-ray diffuse background in the energy range 0.1–2.0 keV is reviewed. A consistent model, based on the soft X-ray brightness distribution and the energy spectrum over the sky, is derived. The observed diffuse background is predominantly of galactic origin and considered as thermal emission for the most part from a local hot region of temperature ≈10⁶ K which includes the solar system. Several pronounced features of enhanced emission are interpreted in terms of hot regions with temperatures up to 3×10⁶K, some of which are probably old supernova remnants. The properties of the soft X-ray emitting regions are discussed in relation to the observational results on O vi absorption.     

Dielectronic satellite spectra in the soft X-ray region

Satellite lines, situated on the long wavelength side of the helium-like ion resonance line, can be observed in highly-ionized ions both in laboratory sources and from the Sun. Although seen for more than 30 years, these lines have only recently been classified in detail as inner-shell transitions in lithium-like ions. Laboratory experiments have shown that under steady-state conditions these satellites are produced by dielectronic recombination, although in transient ionizing plasmas direct inner-shell excitation can be important. Detailed calculations have been carried out for high Z ions up to copper, and the results can be compared with solar flare spectra in iron. Such comparisons allow both the electron temperature and the transient state of the plasma to be determined. Laboratory spectra from such high-Z ions are different in appearance, and may be dominated by processes resulting from the transient ionizing state of the plasma.     

The soft X-ray spectrum of NGC 4151

EXOSAT observations of the Seyfert galaxy NGC 4151 over the period July 1983 to April 1984 have revealed a decreasing flux in the 2 –10 keV band. In accord with previous measurements a power law spectrum attenuated with a simple column of cold gas does not provide a satisfactory spectral fit below 3 keV, where a lower relative opacity is required. Inclusion of additional low energy data from the EXOSAT telescopes allows the modelling of the absorbing column to be improved and reveals a second, separate, soft X-ray spectral component.     

Ariel VI soft X-ray observations of Cygnus X-1

Observations of Cygnus X-1 during the high-low transition of June–July 1980 reveal an intense flux between 0.5 and 1.5 keV. Although the intensity broadly follows the 1–12 keV flux through the transition, there is no evidence of variations in the shape of the energy spectrum. The implications of these results and derived limits on the minute-to-minute variability are discussed.     

A study of volume versus frequency for soft switching IGBTconverters

Earlier references have described a new soft switched ZVS/ZCS (zero voltage switching, zero current switching) converter for IGBTs that allows operation above 20 kHz. Although frequencies above 20 kHz are now possible for IGBT converters, the optimum frequency for minimum volume may be below 20 kHz because of heat sink requirements. A comparative study considers the reactive component versus heat sink volume tradeoff for two 6 kW converters, one using ZVS/ZCS and the other using a more conventional circuit with hard switching     

Variability of soft X-ray emission of EX Hydrae observed with Einstein Observatory

The cataclysmic variable EX Hydrae has been observed in X-rays with Einstein Observatory. A 67 min periodic X-ray modulation has been found in the energy range. 1 – 2 keV, whereas the source is approximately constant above 2 keV. The modulation is approx. in phase with the stable 47 min modulation in the optical brightness. The X-ray spectrum changes slightly with the 67 min phase but is consistent with a two component model with constant temperature only changing in relative intensity. Quasi-simultaneous optical observations were also obtained and used to extend the time base of the optical modulation. The result is indicative of a decrease in the 67 min period on a time scale of 3 10⁶ yr. The implications for the hypothesis of a non-uniform rotating white dwarf as the origin of the 67 min optical and X-ray modulation are discussed.     

Be stars in young clusters in the Magellanic Clouds

A substantial fraction (typically 10%) of Galactic B stars consists of Be stars. While Galactic Be stars have been fairly well investigated, very little is known about the Be star content of the Magellanic Clouds (MCs). We present a refined method of Be star identification by CCD photometry and apply it to four young clusters and associations in the MCs. We find NGC 330 in the SMC to be exceptionally rich in Be stars, while the fraction is clearly lower in the similarly aged LMC clusters NGC 2004 and NGC 1818. NGC 2044, a very young region in the LMC, contains almost no Be stars. Among very early-type B stars in the investigated MC clusters we find the largest number of Be stars, while in the Milky Way this is shifted to somewhat later types. In the LMC, there may be a second frequency peak around B6.Based on observations obtained at the 2.2m MPIA telescope at ESO, La Silla, Chile, partly on time granted by the MPIA, Heidelberg.     

O-star winds in the Magellanic Clouds and the Milky Way

UV P-Cygni profiles of OB-stars in the Magellanic Clouds (observed with HST), and the galaxy (observed with IUE) are analyzed empirically using a line formation procedure similar to the one described by Lamers et al. (1987). The assumption of a constant microturbulencev _turb throughout the wind is dropped and replaced by a radially increasing turbulence parameterv _turb(v), thus improving the fit for the emission peaks substantially, and at the same time avoiding the need for a justification of extremely supersonic turbulence in the vicinity of the wind's sonic point. The Sobolev optical depth is determined interatively at fixed velocities in the wind, which removes the bias introduced by the choice of a specific parameterization function. Where it was possible and necessary a full photospheric spectrum was used to illuminate the wind line. The terminal velocitiesv are are found to be largest in the Galaxy, smallest in the Small Magellanic Cloud, and intermediate or similar to galactic in the Large Cloud.     

The massive star distribution in the Galaxy and the Magellanic Clouds

The numbers and distribution of Population I O-type stars and Wolf-Rayet stars are reviewed. The numbers of known WR stars in the Galaxy, the LMC and the SMC are 185, 114, and 9, respectively. Distances and galactic distributions determined by various authors are compared. The single star and binary distributions are discussed in the light of evolutionary studies.     

Hubble Space Telescope spectroscopy of massive hot stars in the Magellanic Clouds and M31

Using the Hubble Space Telescope (HST) and the Faint Object Spectrograph (FOS) high signal to noise spectrograms were obtained for 15 OB stars in the Magellanic Clouds^***, three of which are of spectral type O3. The data cover the spectral region from 1150 A – 2300 A with a resolution of /1 A. One O8.5 supergiant, OB78#231, in M31is also included in this work. These data are a substantial improvement on previous high resolution IUE observations in the Magellanic Clouds (Walborn et al. 1985 and references therein) because of the smaller aperture and the much better signal to noise ratio, while no high resolution UV spectra of O stars in M31 have been obtained before. In this paper we discuss various morphological aspects of the spectra, concerning metallicity and the stellar winds, compared to galactic analogues.     

一种个性化标签云中的标签排序算法

社会化标签能够直接反映用户兴趣和商品特征,因而可用于个性化推荐系统中。使用标签进行推荐时,需要将其排序,而现有标签云中的标签排序都是按标签被标记次数或字典顺序进行降序排列的,这些排列方式未考虑用户个性化的需求和标签的时效性。提出了一种个性化标签云中的标签排序算法,通过用户自身的兴趣与挖掘出的用户潜在兴趣进行标签排序,从而构建个性化的标签云,并根据用户兴趣的变化定期对标签云进行更新,可以更好地发现电子商务网站中用户感兴趣的商品。实验对比结果表明,个性化标签云中的标签排序算法能够有效的提高商品推荐质量。     

基于微处理器的大数及其计算方法研究

主要研究了无需限位的不定长二进制浮点数及其计算方法。给出了基于原码的不定长二进制浮点数的表示方法,并以加法和移位等逻辑算法为基础,总结出了不定长二进制浮点数四则运算的通用计算方法并给出计算实例,从而实现超长二进制浮点数的计算。     

一种摆式大量程加速度计的设计

介绍了一种摆式大量程加速度计的工作原理.基于经典控制理论完成了加速度计各环节数学模型的建立,对加速度计悬丝支承、力矩器、位移传感器、伺服电路等部件进行了说明,阐述了该大量程加速度计的技术特点.     

OpenGVS中三维云的快速模拟

三维云的模拟可以大大提高飞行模拟器视景的逼真度,粒子系统又是模拟三维云的有效方法.介绍了三维视景中模拟三维云的几种常用方法,分析了OpenGVS中仿真云的局限性以及粒子系统模拟三维云的优点,在分析粒子系统的基础上,提出了一种在OpenGVS中基于灰度图约束的模拟三维云的方法,利用该算法,通过恰当选择粒子数量和粒子模型可以在取得逼真效果的同时满足视景系统实时性的要求.最后给出了在OpenGVS中的实现方法.