银河系中心超大质量黑洞Sgr A＊的光变研究进展

越来越多的观测证据表明,位于银河系中心的致密射电源SgrA*是一个质量约为400万个太阳质量的超大质量黑洞.本文介绍在射电、毫米/亚毫米、近红外、X射线波段对Sgr A*的光变观测和理论研究进展.自1974年被射电干涉测量发现伊始,Sgr A*就被检测到时标从天到年不等的射电光变,随着新的观测设备的出现和观测技术的发展,天文学家先后在所有的对银河系中心可观测波段上检测到了Sgr A*的光变,包括在毫米/亚毫米波段的时标为小时的快速光变,近红外波段上时标不到1 h的显著光变,以及空间X射线卫星记录到的幅度变化几十倍以上的巨大耀变.这些光变观测数据可以用于估算产生Sgr A*耀变辐射的区域范围(假设光变是由整个源产生的,辐射区域的尺度/与光变时标τ之间存在线性关系,/≤Cr),并对Sgr A*辐射机制研究提供了间接的限制.近年来开展的一些多波段联测显示,近红外和×射线光变是同步发生的,并且都比射电和毫米波光变先出现,这类时间延迟支持Sgr A*光变的绝热膨胀理论模型.但目前成功的多波段耀变观测非常有限,如何获得从射电厘米波到X射线的Sgr A*光变间的内在关联将是未来几年中Sgr A*光变的一个主要研究方向.     

A^＊算法软件构件的研究

提出了一种以软件构件形式实现A^*算法的方案，用面向对象的方法，以状态描述为基础，对A^*算法数据集进行抽象，将A^*算法设计成抽象类，这一抽象类可通过继承和重写应用于不同的环境，从而提高了A^*算法软件的可重用性。     

投影算子的Faddeev型算法的改进

给出了投影算子PAT,S与PT,（A^*S）的改进算法。     

用加权MP逆的定义方程推导[A，B]NM＋的显式

利用加权Moore-Penrose逆AMN^ 的定义方程A^*MAX=A^*M，R(X)真包含N^-1R(A^*)简捷地导出了[A，B]NM^ 的显式，并给出了它的两种变型．     

上海天文台并址站的空间归心测量

上海天文台佘山站的SLR（激光测卫），VLBI（甚长基线干涉测量）和GPS（全球定位系统）站是国际上用以建立和维持ITRF（international terrestrial reference frame，国际地球参考框架），进行全球天文地球动力学研究的基准台站之一．联合应用这些空间测量，需要知道这三个站心间精确的三维相对位置．为此重点介绍了高精度确定VLBI，SLR几何旋转中心的观测方案和计算方法，归心结果经比较达到了1cm的外附精度，为国内其他并址VLBI，SLR和GPS台站的空间归心测量提供了先例．     

C*代数的对偶

设A是可分的交换C^*－代数,A^*是其对偶,证明了A^*＝Ω的复线性W^*－闭张,其中Ω是A的谱空间。     

分块矩阵广义逆的几种表达式

受分块矩阵的逆矩阵形式的启发，给出了分块矩阵A=（A11 A12 A21 A22）的广义逆A^（1，3），A^（2），A^＋，Ad和Ag可以表示为X=（S1^α-A11^αA12S2^α -A11^αA21S1^α S2^α）的条件；然后运用这些结果，得到分块矩阵A的M—P逆的几个表达式；最后给出一个求分块矩阵M—P逆的例子．     

基于A*算法的启发式算法求解多序列比对问题

通过分析动态规划算法及A^*算法的特点，针对多序列比对问题提出一种基于A^*算法的启发式算法。该算法采用了多个优化搜索机制。通过对此算法的理论分析，证明了它能够在有效地减小搜索的空间、节约搜索的时间的同时，保证得到比较好的比对结果。此算法不仅能够在多序列比对问题中得到应用，还能够用于其他有向无环图的最短路径问题的求解。     

伴随阵与两种广义逆阵的若干性质

设anjA,A^ ,A^D分别表示复方阵A的伴随阵，Moore-Penrose逆和Drazin逆，利用矩阵的奇异值分解，约当分解和极限过程的方法，证明了：（adjA)^ =adj(A^ ）,(adjA)^D=adj(A^D），并得到当A是复亚半正定阵时，A^ 和A^D也均为复亚半正定阵，且A^ =A^D。     

基于L^＊系统的一种非单调推理系统

研究了非单调优先推理系统P和累积单调推理系统CM，以及模糊命题演算的形式演绎系统L^*，在L^*系统中定义了后承关系|～：A|～B当且仅当A^2┠B，证明了在L^*系统中的这种后承关系满足累积单调推理系统CM，非单调优先推理系统P的全部规则，但这种后承关系不满足单调推理系统M的逆否律规则，从而在L^*系统中建立了一个介于非单调推理系统和单调推理系统之间的逻辑系统，这为两种系统的理论研究建立一个桥梁以及为模糊控制提供了一种新的思路。     

A size of approximately 1 au for the radio source Sgr A* at the centre of the Milky Way

Although it is widely accepted that most galaxies have supermassive black holes at their centres, concrete proof has proved elusive. Sagittarius A* (Sgr A*), an extremely compact radio source at the centre of our Galaxy, is the best candidate for proof, because it is the closest. Previous very-long-baseline interferometry observations (at 7 mm wavelength) reported that Sgr A* is approximately 2 astronomical units (au) in size, but this is still larger than the 'shadow' (a remarkably dim inner region encircled by a bright ring) that should arise from general relativistic effects near the event horizon of the black hole. Moreover, the measured size is wavelength dependent. Here we report a radio image of Sgr A* at a wavelength of 3.5 mm, demonstrating that its size is approximately 1 au. When combined with the lower limit on its mass, the lower limit on the mass density is 6.5 x 10(21)M(o) pc(-3) (where M(o) is the solar mass), which provides strong evidence that Sgr A* is a supermassive black hole. The power-law relationship between wavelength and intrinsic size (size proportional, variantwavelength(1.09)) explicitly rules out explanations other than those emission models with stratified structure, which predict a smaller emitting region observed at a shorter radio wavelength.     

Event-horizon-scale structure in the supermassive black hole candidate at the Galactic Centre

The cores of most galaxies are thought to harbour supermassive black holes, which power galactic nuclei by converting the gravitational energy of accreting matter into radiation. Sagittarius A* (Sgr A*), the compact source of radio, infrared and X-ray emission at the centre of the Milky Way, is the closest example of this phenomenon, with an estimated black hole mass that is 4,000,000 times that of the Sun. A long-standing astronomical goal is to resolve structures in the innermost accretion flow surrounding Sgr A*, where strong gravitational fields will distort the appearance of radiation emitted near the black hole. Radio observations at wavelengths of 3.5 mm and 7 mm have detected intrinsic structure in Sgr A*, but the spatial resolution of observations at these wavelengths is limited by interstellar scattering. Here we report observations at a wavelength of 1.3 mm that set a size of 37(+16)(-10) microarcseconds on the intrinsic diameter of Sgr A*. This is less than the expected apparent size of the event horizon of the presumed black hole, suggesting that the bulk of Sgr A* emission may not be centred on the black hole, but arises in the surrounding accretion flow.     

A gas cloud on its way towards the supermassive black hole at the Galactic Centre

Measurements of stellar orbits provide compelling evidence that the compact radio source Sagittarius A* at the Galactic Centre is a black hole four million times the mass of the Sun. With the exception of modest X-ray and infrared flares, Sgr A* is surprisingly faint, suggesting that the accretion rate and radiation efficiency near the event horizon are currently very low. Here we report the presence of a dense gas cloud approximately three times the mass of Earth that is falling into the accretion zone of Sgr A*. Our observations tightly constrain the cloud's orbit to be highly eccentric, with an innermost radius of approach of only ～3,100 times the event horizon that will be reached in 2013. Over the past three years the cloud has begun to disrupt, probably mainly through tidal shearing arising from the black hole's gravitational force. The cloud's dynamic evolution and radiation in the next few years will probe the properties of the accretion flow and the feeding processes of the supermassive black hole. The kilo-electronvolt X-ray emission of Sgr A* may brighten significantly when the cloud reaches pericentre. There may also be a giant radiation flare several years from now if the cloud breaks up and its fragments feed gas into the central accretion zone.     

Rapid X-ray flaring from the direction of the supermassive black hole at the Galactic Centre.

The nuclei of most galaxies are now believed to harbour supermassive black holes. The motions of stars in the central few light years of our Milky Way Galaxy indicate the presence of a dark object with a mass of about 2.6 x 106 solar masses (refs 2, 3). This object is spatially coincident with the compact radio source Sagittarius A* (Sgr A*) at the dynamical centre of the Galaxy, and the radio emission is thought to be powered by the gravitational potential energy released by matter as it accretes onto a supermassive black hole. Sgr A* is, however, much fainter than expected at all wavelengths, especially in X-rays, which has cast some doubt on this model. The first strong evidence for X-ray emission was found only recently. Here we report the discovery of rapid X-ray flaring from the direction of Sgr A*, which, together with the previously reported steady X-ray emission, provides compelling evidence that the emission is coming from the accretion of gas onto a supermassive black hole at the Galactic Centre.     

Near-infrared flares from accreting gas around the supermassive black hole at the Galactic Centre

Recent measurements of stellar orbits provide compelling evidence that the compact radio source Sagittarius A* (refs 4, 5) at the Galactic Centre is a 3.6-million-solar-mass black hole. Sgr A* is remarkably faint in all wavebands other than the radio region, however, which challenges current theories of matter accretion and radiation surrounding black holes. The black hole's rotation rate is not known, and therefore neither is the structure of space-time around it. Here we report high-resolution infrared observations of Sgr A* that reveal 'quiescent' emission and several flares. The infrared emission originates from within a few milliarcseconds of the black hole, and traces very energetic electrons or moderately hot gas within the innermost accretion region. Two flares exhibit a 17-minute quasi-periodic variability. If the periodicity arises from relativistic modulation of orbiting gas, the emission must come from just outside the event horizon, and the black hole must be rotating at about half of the maximum possible rate.     

Improvement of orbit determination for geostationary satellites with VLBI tracking

China’s COMPASS satellite navigation system consists of five or more geostationary (GEO) satellites.The roles of GEO satellites are to improve the regional user’s positioning accuracy and provide the continuous Radio Determination Satellite Service.The motion of GEO satellites relative to a ground tracking station is almost fixed,and regular orbit maneuvers are necessary to maintain the satellites’ allocated positions above the equator.These features present difficulties in precise orbit determination (POD).C-band ranging via onboard transponders and the L-band pseudo-ranging technique have been used in the COMPASS system.This paper introduces VLBI tracking,which has been successfully employed in the Chinese lunar exploration programs Chang’E-1 and Chang’E-2,to the POD of GEO satellites.In contrast to ranging,which measures distances between a GEO satellite and an observer,VLBI is an angular measurement technique that constrains the satellite’s position errors perpendicular to the satellite-to-observer direction.As a demonstration,the Chinese VLBI Network organized a tracking and orbit-determination experiment for a GEO navigation satellite lasting 24 h.This paper uses the VLBI delay and delay-rate data,in combination with C-band ranging data,to determine the GEO satellite’s orbit.The accuracies of the VLBI delay and delay rate data are about 3.6 ns and 0.4 ps/s,respectively.Data analysis shows that the VLBI data are able to calibrate systematic errors of the C-band ranging data,and the combination of the two observations improves orbit prediction accuracy with short-arc data,which is important for orbital recovery after maneuvers of GEO satellites.With the implementation of VLBI2010,it is possible for VLBI to be applied in the COMPASS satellite navigation system.     

An analysis of the polar motion series from VLBI observations

From the reduction of 2893 globally distributed astrometric and geodetic VLBI sessions from August 1979 to the end of 1998, coordinates of 722 radio sources at J2000.0, coordinates and velocities of 128 stations at J1997.0 and about 20 years Earth Orientation Parameters were estimated. From the analysis of the resultant polar motion series, the following are demonstrated: (ⅰ) During the VLBI data span the Markowitz wobble is not exhibited. (ⅱ) The amplitudes of both annual and Chandler wobble show temporal variations, with the former being more obvious than the latter. (ⅲ) Wavelet analysis shows that all the signals in the polar motion series are characterized by temporal variation in amplitudes. If we take any signal as strictly periodic, it is impossible to remove it completely from the polar motion series by least-squares fit because the hypothesis of a constant amplitude conflicts with VLBI measurements. (ⅳ) By applying a filter, the secular polar motion was found to be (2.74±0.01) mas/a towards (83.9±0.3) °W longitude, which is smaller in rate and more westward in direction compared with those determined from optical observations or the combination of optical and space geodetic observations.     

Determination of the controlled landing trajectory of Chang’E-1 satellite and the coordinate analysis of the landing point on the Moon

Based on the tracking observations of radio ranges and VLBI delays of Chang’E-1 (CE-1) satellite during the controlled landing on the Moon on March 1, 2009, the landing trajectory and the coordinates of the landing point are determined by positioning analysis. It is shown that the landing epoch (the emission epoch of the last signal) of CE-1 satellite on the Moon was at UTC8h13m6.51s. The lunar longitude, latitude and surface height of the landing point in the lunar primary axes frame are respectively 52.27...     

Investigation of stronger diurnal ERP signals in summer derived from the VLBI CONT08 campaign

A series of very successful Continuous Very Long Baseline Interferometry Campaigns (CONT) have been carried out at irregular intervals since 1994. One of the goals is to support high-resolution earth rotation studies. The most recent CONT08 campaign was conducted with a network of 11 observatories at an increased recording rate of 512 Mbit per second over a fortnightly time span, from which stronger diurnal variations of the Earth Rotation Parameters (ERP) have been detected. We compared the high-frequency ERP from VLBI and GPS observations during CONT02, CONT05 and CONT08 with the atmospheric angular momentum functions derived from the National Centers for Environmental Prediction/National Center for Atmospheric (NCEP/NCAR) during these periods. We attribute the detected diurnal discrepancies between the theoretical models and the CONT08 observations to atmospheric excitations.