人造地球卫星变轨问题的分析与探讨

通过借助导出的在极坐标系下物体在万有引力作用下运行的轨道方程,对人造地球卫星的轨道转换进行了定性的分析与探讨.     

施工坐标在特大型桥梁工程施工中的应用

介绍了施工坐标建立方法,施工坐标系与北京坐标系了关系及转换,施工坐标系在桥梁施工中应用优势     

某市地方独立坐标系与独立工程坐标系的转换

坐标第转换是测量中经常需要解决的问题.在小区域范围内,可将地方独立坐标系和工程坐标系视为在平面上建立的坐标系,而不需考虑投影产生的距离和方向变形,从而采用平面上的坐标系相似变换方式实现两个坐标系的想互转换.本文详细叙述了以工程坐标系控制点为重合点,采用坐标系相似变换方法实现某市地方独立坐标系与某企业独立工程坐标系的相互转换.     

轨道机动航天器SINS/GPS自主组合导航算法

为了实现空间机动目标的自主导航,提出了一种基于地心惯性坐标系的轨道机动航天器SINS/GPS自主组合导航算法.首先分析了轨道机动航天器的特点,选取地心惯性坐标系作为导航坐标系.然后建立了导航滤波器的状态方程以及量测方程,其中考虑了SINS系统平台失准角、加速度计误差、陀螺仪误差和加速度计的安装位置和航天器质心之间偏差的影响.最后进行了相关的数学仿真验证,仿真结果表明,该算法可以较准确地给出位置和速度导航信息.     

数控加工中关于工件坐标系建立方法的探讨

工件坐标系是编程人员在编程和加工时使用的坐标系,是程序的参考坐标系。工件坐标系的设定应根据零件特点,利于编程和尺寸的直观性,并且应便于操作人员在机床上找到。本文通过对工件坐标系的分析,提出一种在数控机床上,通过人工快速、准确地建立工件坐标系的方法。     

利用Visual Basic语言在独立坐标系中绘图

在有些实际测量工作中用测量坐标系是很不方便的,为了测量工作的方便将用到独立坐标系进行测量工作,因此需要将测量坐标系转换为独立坐标系。由于测量坐标系和VisualBasic语言中容器的缺省坐标系不同,通过坐标系转换,并利用摘要:VisualBasic语言编写一定的程序进行绘图。     

解析面积坐标系与射影坐标系之间的内在联系

文献[1]中创立了一种很有用的面积坐标,但是未弄清楚面积坐标系与原有的一些坐标系之间的联系,并且出现了“若u1+u2+u3=0,就说(u1: u2: u3)代表一个无穷远点”等错误,本文就这些问题进行解析,并得到结论:面积坐标系就是一种特殊的射影坐标系.     

通用地理坐标转换类设计与实现

为了解决地图制图中不同坐标系之间的相互转换的问题,采用构建通用地理坐标转换类方法,实现常用大地坐标系和平面投影坐标系之间在相同或不同参考椭球参数下的相互转换.介绍了大地坐标系及投影坐标系,对实现大地坐标系、投影坐标系的相互转换方法作了详细的论述,并探讨了通用地理坐标转换类设计和实现的优化方法,通过实际数据验证了该地理坐标转换类在实际的应用中是切实可行的.     

弧焊机器人系统标定

介绍了在研发昆山一号机器人的过程中所设计的标定工具坐标系的七点法和标定工件坐标系的三点法,实现了机器人工具坐标系及工件坐标系的标定.机器人工具坐标系的标定就是确定工具坐标系相对于末端坐标系的齐次转换矩阵.机器人工件坐标系的标定就是确定工件坐标系相对于基坐标系的齐次转换矩阵.通过系统标定,机器人的定位精度达到了±0.5 mm.实际的焊接试验表明该方法是一种可靠简便,精度高的系统标定方法,完全满足实际加工要求.     

斜角坐标系与周角坐标系组合构图形式研究

从理论上探讨了斜角坐标系与周角坐标系量化图形的组合形式,并详细阐述了两种坐标系的构图方法,从而为此类组合图形的实际应用提供了理论依据.     

一个稳态轴对称非Kerr黑洞时空中的粒子能级与非热辐射

黑洞质量多极矩的存在和裸奇点的出现对视界附近的粒子能级分布产生强烈的影响，在非Keer黑洞视界附近有正、负能级交错区，其粒子能级交错区与稳态Kerr黑洞时空中的情形不同，稳态非Kerr黑洞的非热辐射与质量多极矩有关。     

Vaidya黑洞量子热效应再讨论

指出了用内向Eddington坐标研究蒸发型Vaidya黑洞热效应可能出现的困难．通过引入一个坐标变换,新的坐标系下对应的困难消失,在新的坐标系下分别用Damour-Ruffini方法和辐射反作用法重新计算了Vaidya黑洞的温度,并讨论了熵,所得结果是合理的．     

含宇宙项带电时空中旋量粒子的量子效应

从带宇宙项带电时空中的二维线元入手,利用D irac方程研究旋量粒子的Hawk ing效应.研究结果显示,在含有宇宙带电时空中,不仅存在黑洞视界,同时也存在宇宙界且在宇宙附近同样存在类似黑洞视界的Hawk ing辐射,同时也提供了一种研究球对称黑洞性质的新方法.     

广义相对论有效势与伪牛顿有效势的比较

比较了在牛顿力学和广义相对论框架中有效势的特征，对比了广义相对效势和两种伪牛顿有效势（PW有效势力和LC有效势）所对应的最内稳定圆轨道半径和放能效率，结果表明，PW有效势能很好地描述检验粒子在Schwarzschild黑洞赤道面上的轨道特征，LC有效势也能较好地模拟检验粒子在Kerr黑洞赤道面上的轨道特征（顺行粒子向快转黑洞吸积的情况除外）。     

The accelerations of stars orbiting the Milky Way's central black hole

Recent measurements of the velocities of stars near the centre of the Milky Way have provided the strongest evidence for the presence of a supermassive black hole in a galaxy, but the observational uncertainties poorly constrain many of the black hole's properties. Determining the accelerations of stars in their orbits around the centre provides much more precise information about the position and mass of the black hole. Here we report measurements of the accelerations of three stars located approximately 0.005 pc (projected on the sky) from the central radio source Sagittarius A* (Sgr A*); these accelerations are comparable to those experienced by the Earth as it orbits the Sun. These data increase the inferred minimum mass density in the central region of the Galaxy by an order of magnitude relative to previous results, and localize the dark mass to within 0.05 +/- 0.04 arcsec of the nominal position of Sgr A*. In addition, the orbital period of one of the observed stars could be as short as 15 years, allowing us the opportunity in the near future to observe an entire period.     

带有整体磁单极子的Reissner-Nordstrom黑洞的隧道效应

将Parikh的工作推广到带有整体磁单极子的R-N黑洞,其特点是ADM质量不等于黑洞的质量参数,需要改变一个常数.通过将Hawking辐射看成是穿过事件视界的隧道效应,计算出隧道穿透率并且得到了一个相对于半经典穿透率的修正.     

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.     

Garfinkle-Horowitz-Stromingen dilaton黑洞的Hawking隧穿辐射

用量子隧穿法研究Garfinkle—Horowitz—Stromingen dilaton黑洞的Hawking辐射,得到了静止质量为零和不为零的两类粒子穿过黑洞事件视界的出射率,发现粒子的量子隧穿辐射谱与黑洞的Bekenstein—Hawking熵变有关,辐射谱不再是严格的纯热谱．     

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.     

黑洞视界面积定理

从满足Nernst定理的黑洞熵与视界面积的关系得出黑洞视界面积定理:满足Nernst定理的黑洞熵与其全面积成正比;对于单视界黑洞,其全面积即视界面积;对于双视界黑洞,其全面积为内、外视界面积的代数和;黑洞具有物理意义的视界不多于两个。