生物组织光学参数：优化散射系数（μ’s）的实时在位测定

利用了一套特殊设计光纤探头组成的稳定态光纤光谱仪测试生物组织的光学参数，从悬乳液(Intralpid)与模拟胶(Phantom)实验推导出优化散射系数(Reduced scattering coeffcient：μ’s)近红外谱测量经验公式。测量反射系数就可以计算出优化散射系数谱。计算结果用模拟胶作了验证，并对大鼠脑组织μ’s进行了实时在位测量，从而得到了一种μ’s在位测量的有效方法。     

彩色三维激光快速成型技术的研究

目前逆向工程采用线结构激光和一个彩色面阵CCD摄像机构成三维彩色扫描系统,彩色CCD摄像机分两次对被测物体成像,首先摄取物体的彩色图片,然后加用滤光片再摄取激光光平面上的三维信息.最后将两次获取的信息重叠,便可得到三维彩色信息.提出了激光光平面方程式三维测量方法,建立了相应的数学模型.研制成一套适用于彩色逆向工程流程,并进行了实验研究,给出了实验结果.     

太阳微波爆发精细结构与硬X射线耀斑的相关

北京天文台在２．８４ＧＨｚ频率上观测到的带短时标精细结构的微波爆发与日本ＹＯＨＫＯＨ卫星上ＨＸＴ在１９９１年１０月－１９９２年１２月观测到的硬Ｘ射线爆发（ＨＸＢ）事件作了比较，发现在２０个微波精细结构爆发事件只有１２个与ＹＯＨＫＯＨ卫星记录的ＨＸＢ有对应关系．本文对１９９２年６月７日典型事件中２．８４ＧＨｚ与ＨＸＢ共同存在的百秒量级的准周期振荡作了分析及源区参数的计算，并作了简要的讨论．     

X-ray synchrotron nebulae and the origin of neutron stars

“With all reserve, we advance the view that a supernova represents the transition of an ordinary star into a neutron star.”This conclusion, reached just 50 years ago in a classic paper by Walter Baade and Fritz Zwicky (1934), was published three decades before the first direct observational evidence for the existence of neutron stars was uncovered. It still informs the standard picture of neutron star production in the Galaxy. We examine herein some recent evidence bearing on this question which has been derived from Observatory X-ray observations of supernova remnants and radio pulsars. In particular, the discovery that X-ray synchrotron nebulae are found surrounding most young ( 10⁶ yr) pulsars observed to date is discussed. We explore the implications of the lack of such nebulae in the majority of supernova remnants (SNR) for the properties and frequency of neutron star formation in supernova events.     

Magnetar spectra and twisted magnetospheres

The huge potential drop between the footpoints of the closed field lines in the twisted magnetospheres of magnetars may accelerate electrons up to very high energies, γ ? 10⁶. On the other hand, the comparison between the observed spectra of magnetars and spectra obtained by accurate theoretical models seems to favor of a picture in which the magnetosphere is filled by “slow” electrons (v ? 0.8c), rather than by ultra-relativistic particles.     

Modeling the broadband persistent emission of magnetars

In this paper, we discuss our first attempts to model the broadband persistent emission of magnetars within a self-consistent, physical scenario. We present the predictions of a synthetic model that we calculated with a new Monte Carlo 3D radiative code. The basic idea is that soft thermal photons (e.g. emitted by the star surface) can experience resonant cyclotron upscattering by a population of relativistic electrons treated in the twisted magnetosphere. Our code is specifically tailored to work in the ultra-magnetized regime; polarization and QED effects are consistently accounted for, as well different configurations for the magnetosphere. We discuss the predicted spectral properties in the 0.1–1000 keV range, the polarization properties, and we present the model application to a sample of magnetars soft X-ray spectra.     

A fast pulse phase estimation method for X-ray pulsar signals based on epoch folding

X-ray pulsar-based navigation (XPNAV) is an attractive method for autonomous deep-space navigation in the future. The pulse phase estimation is a key task in XPNAV and its accuracy directly determines the navigation accuracy. State-of-the-art pulse phase estimation techniques either suffer from poor estimation accuracy, or involve the maximization of generally non-convex object function, thus resulting in a large computational cost. In this paper, a fast pulse phase estimation method based on epoch folding is presented. The statistical properties of the observed profile obtained through epoch folding are developed. Based on this, we recognize the joint prob-ability distribution of the observed profile as the likelihood function and utilize a fast Fourier transform-based procedure to estimate the pulse phase. Computational complexity of the proposed estimator is analyzed as well. Experimental results show that the proposed estimator significantly outperforms the currently used cross-correlation (CC) and nonlinear least squares (NLS) estima-tors, while significantly reduces the computational complexity compared with NLS and maximum likelihood (ML) estimators.     

ASTROSAT

The ASTROSAT satellite is an Indian National Space Observatory under development in India. Due for launch in 2010, ASTROSAT will carry a complement of five scientific instruments enabling simultaneous observations from the optical through to the hard X-ray energy band. This capability will enable broad-band spectroscopy and high time-resolution monitoring of both galactic and extra-galactic targets, such as X-ray binaries and AGN. One of the instruments is being built in collaboration with the Canadian Space Agency and another in collaboration with the University of Leicester. ASTROSAT also carries a scanning sky monitor to observe the variable X-ray sky. After an initial period of science verification and guaranteed time, a certain fraction of ASTROSAT observing time will also be made available to the community via a call for proposals. Here I summarise the instrument complement and principle scientific objectives of the mission.     

应用PIV技术测试模型环形燃烧室流场

采用粒子图像测速仪(PIV)测量带双级旋流器模型环形燃烧室内冷态和燃烧流场,试验研究不同进口气流温度对其冷态和燃烧流场内回流区的形成以及气流速度分布的影响,试验结果表明:燃烧室燃烧流场内回流区长度要比冷态流场短,燃烧流场的脉动速度明显大于冷态流场;另外随着进口气流温度增加,燃烧室冷态和燃烧流场的回流区长度都稍有减少.      

对地观测卫星成像调度的多目标约束修正方法

 约束修正是对地观测卫星成像调度的重要组成部分,负责处理成像调度方案的约束满足与优化,是一类复杂的组合优化问题。为得到优化可行的成像调度方案,提出一种新的约束修正方法。针对约束修正问题构建时间序有向图模型,并将约束修正问题归结为点带约束成本的优化路径搜索问题;在此基础上,提出一种基于标记更新的多目标约束修正算法。实际问题的实验与分析表明：该方法能够在规定的时间内求得问题所有的多目标优化解,有效地解决了卫星成像调度的约束满足与优化问题。