共查询到20条相似文献，搜索用时 62 毫秒
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《天文学报》2016,(5)
天体测量法是探测系外行星一种有效的手段,具有其他探测方法所不具备的独特优势,如可以探测到行星的3维轨道参数及确定行星的质量等,这些将为现有的行星样本提供重要补充.高精度的空间天体测量卫星Gaia(Global Astrometric Interferometer for Astrophysics)在2013年成功发射升空,可以预期未来基于其探测数据,将可能发现大量的长周期类木行星.针对αCentauri A、HD 62509和GJ 876系统,根据Gaia单次天体测量精度生成对应的仿真数据,使用Lomb-Scargle周期谱分析行星轨道周期信号,并采用Markov Chain Monte Carlo(MCMC)算法对行星系统进行轨道反演,得到的结果与行星的初始参数相吻合. 相似文献
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《天文学报》2017,(6)
系外类地行星空间探测计划(Search for Terrestrial Exo-Planets,以下简称"STEP")采用天体测量法和微像素级焦平面定标测量技术,设计望远镜焦平面检测精度达到1μas.在假定焦平面设计能达到检测精度的前提条件下,系统分析了恒星自行、视差、卫星速度和位置、光学系统的光心等关键因素对检测系外行星的影响.有别于传统的窄视场照相底片常数法,提出了一种恒星相对角距测量方法,以检测由于可能存在的系外行星而引起星对角距变化的非线性项,消除了传统窄视场天体测量中参考星位置和自行精度对检测系外行星的直接影响.针对同一天区内的8颗参考星和1颗具有行星系统的待测星,分别模拟出5 yr内的观测数据,利用最小二乘法进行处理,发现基于STEP自身1μas的观测精度,在这种情况下是可以观测到类地行星的. 相似文献
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介绍了国际测地/天体测量学甚长基线干涉测量服务(International Very Long Baseline Interferometry (VLBI) Service for Geodesy and Astrometry, IVS)组织机构及下属分析中心概况.系统归纳了目前IVS发布的地球定向参数(Earth Orientation Parameters, EOP)产品类型及不同观测类型的用途.利用2010—2019年公开发布的观测资料,对IVS不同分析中心的EOP日常监测和服务能力进行了评估.通过构造观测台站所构成的几何体积,分析了EOP精度与测站数量、测站网分布的关系,统计了IVS不同观测类型的EOP解算精度.此外,综合公开发布的美国、欧洲等区域网观测数据,分析了不同地区区域网的常规及加强观测结果与IVS结果的差异.结果表明:EOP的解算精度与观测台站的分布密切相关, IVS常规观测确定的极移分量的外符合精度优于0.2 mas,世界时(Universal Time, UT1)与协调世界时(Coordinated Universal Time,UTC)之差(UT1-UTC)的精度在0.015 ms左右,加强观测的UT1-UTC值与国际自转服务组织(International Earth Rotation Service, IERS)的C04之间存在0.02–0.03 ms的差异.区域观测网的精度受观测网形和基线长度制约,总体劣于IVS观测精度,其中,美国甚长基线干涉阵列(Very Long Baseline Array, VLBA)的常规及加强观测结果与IVS全球观测结果最接近. 相似文献
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激光天文动力学引力波探测任务ASTROD-GW(ASTROD[AstrodynamicalSpace Test of Relativity Using Optical Devices Optimized for Gravitation WaveDetection)是ASTROD专注于探测引力波的优化方案,其航天器轨道在日地拉格朗日点L_3、L_4、L_5附近,构成一个接近等边的三角形阵列,干涉臂长约为2.6×10~8 km,其可探测的引力波波长可达LISA(Laser Interferometer Space Antenna)的52倍.文中综述ASTROD-GW轨道的设计和优化方法.轨道经优化后,其臂长差(在激光干涉测量中可称为干涉差)10 yr内的变化为10~(-4) AU量级、3个臂长方向的多普勒速度小于4 m/s,均小于LISA的要求,因此LISA发展的激光测距技术可用于ASTROD-GW. 相似文献
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空间碎片对人造卫星和飞船的威胁日益增长.为了保持一个安全的空间环境,需要寻找成本低而又准确的空间天体探测和追踪方法.前些年,使用射电望远镜作为被动雷达,探测空间碎片反射的调频广播信号的可能性已经被讨论过,并且月球和国际空间站反射的信号已经被默奇森大视场射电阵(MWA)探测到.介绍MWA探测到的卫星反射广播信号事件,论证MWA有能力探测600 km高度处0.1 m量级大小的空间碎片,位置误差在10 km左右. 相似文献
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预计Hipparcos测定星位的精度要远好于地面仪器的结果。对于从事地面仪器测量的天体测量学家来说,必须回答:地面仪器还能发挥什么作用?我们认为,地面仪器在未来建立惯性坐标系中仍起着重大作用。因为:1.地面经典仪器有相当长的观测历史,因此,在自行方面,有较好地面仪器观测历史的天体其精度并不亚于Hipparcos的结果。2.地面仪器观测可研究与地球物理有关的问题.3.空间卫星不可能包罗全部课题,仍有大量的课题需要地面仪器去观测。4.地面仪器研究课题的运转周期短。一般来说,空间观测的课题要10年以上的周期。5.地面仪器的改造,使得效率和精度有相当大的提高,特别是CCD探测器在天体测量上的应用。中国与丹麦合作的水平子午环,其有效口径为240mm,可观测到13~m.5的天体,因此我们的仪器将在惯性坐标的建立中发挥作用。根据本仪器的特点,可在下列课题发挥其作用:1.观测射电星,作参考系联结的工作。2.观测较暗的小行星,进行坐标系分点改正的工作。3.进行IRS星的绝对测定。4.观测射电源周围的天体,作为观测射电源的定标垦。5.改进FK5星的位置精度。本文发表于IAU141讨论会,1989年10月,列宁格勒。 相似文献
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《中国科学院上海天文台年刊》2014,(0)
空间目标包括在轨卫星、空间碎片等,对其测定轨是空间攻防和空间利用的重要前提。由于地面测站资源有限,单站测量是目前对空间目标尤其是空间碎片测定轨较常用的方式。卫星激光测距(satellite laser ranging,SLR)技术测量精度很高,可达米级(非合作目标),甚至厘米级(合作目标),但不能单独用于单站短弧定轨;电荷耦合器件(charge coupled device,CCD)天文定位技术可观测距离较远的目标,但测量精度为角秒级,换算至空间距离不如SLR技术高。两者的联合为空间目标的高精度定位和跟踪提供了可能,并成为未来空间目标地基测量的发展方向。作为空间碎片单站监测的前期工作,对合作目标的单站定轨精度进行了评估。处理了1500 km高AJISAI低轨卫星的实测数据,分析了单站CCD测角和激光测距数据对低轨空间目标的联合定轨能力,并充分考虑两类不同类型观测数据的精度,数据综合时对其进行合理加权。利用全球激光站资料进行精密定轨,并以此作为参考轨道,采用上海佘山站AJISAI卫星2010年、2011年4天6圈的实测激光测距数据,以及CCD测角数据,开展了单站单圈和单站多圈定轨和预报试验。试验结果表明,测距数据的加入对定轨精度和24小时预报精度的改善非常明显,可提高至少一个数量级;单站单圈联合定轨和24小时预报的精度分别为20 m以内及数百米,单站多圈联合定轨和24小时预报的精度分别在米级及数十米。期望实验结果为中国未来的空间碎片望远镜建设提供参考。 相似文献
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Solar System Research - Finding and studying possible collisions of asteroids approaching the Earth requires a significant amount of computation. This paper describes the R0 program created to... 相似文献
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Magnetars are the neutron stars with the highest magnetic fields up to 1015–1016 G. It has been proposed that they are also responsible for a variety of extra-galactic phenomena, ranging from giant flares in nearby galaxies to fast radio bursts. Utilizing a relativistic mean field model and a variable magnetic field configuration, we investigate the effects of strong magnetic fields on the equation of state and anisotropy of pressure of magnetars. It is found that the mass and radius of low-mass magnetars are weakly enhanced under the action of the strong magnetic field, and the anisotropy of pressure can be ignored. Unlike other previous investigations, the magnetic field is unable to violate the mass limit of the neutron stars. 相似文献
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P. Maltby 《Solar physics》1972,26(1):76-82
Observations of the penumbral intensity of sunspots in 13 wavelength regions are presented. In 4 wavelength regions 54 sunspots are measured. In the other wavelength regions the number of sunspots considered ranges from 3–19.The penumbral intensity alters with position within the spot. This intensity variation is found to be comparable with the change in intensity from one spot to another. The penumbral intensity is found to be independent of spot size in the sample considered.The penumbra model of Kjeldseth Moe and Maltby (1969) with = 0.055 is supported by the measurements. 相似文献
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Many asteroids with a semimajor axis close to that of Mars have been discovered in the last several years. Potentially some of these could be in 1:1 resonance with Mars, much as are the classic Trojan asteroids with Jupiter, and its lesser-known horseshoe companions with Earth. In the 1990s, two Trojan companions of Mars, 5261 Eureka and 1998 VF31, were discovered, librating about the L5 Lagrange point, 60° behind Mars in its orbit. Although several other potential Mars Trojans have been identified, our orbital calculations show only one other known asteroid, 1999 UJ7, to be a Trojan, associated with the L4 Lagrange point, 60° ahead of Mars in its orbit. We further find that asteroid 36017 (1999 ND43) is a horseshoe librator, alternating with periods of Trojan motion. This asteroid makes repeated close approaches to Earth and has a chaotic orbit whose behavior can be confidently predicted for less than 3000 years. We identify two objects, 2001 HW15 and 2000 TG2, within the resonant region capable of undergoing what we designate “circulation transition”, in which objects can pass between circulation outside the orbit of Mars and circulation inside it, or vice versa. The eccentricity of the orbit of Mars appears to play an important role in circulation transition and in horseshoe motion. Based on the orbits and on spectroscopic data, the Trojan asteroids of Mars may be primordial bodies, while some co-orbital bodies may be in a temporary state of motion. 相似文献
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In the text-books of astronomy, sections generally related to the Moon deal with the orbital elements of the Earth-Moon system such asa, e, i, ,
and the time of perigee passage. While the MEAN of the first of the three elements do not vary, mean longitude of the ascending node-mean longitude of the lunar perigee and the time of perigee passage undergoes secular as well as periodic changes due predominantly to the action of the Sun's gravitational attraction. While to a certain degree, explanations related to the calculation of the lunar orbit parameters are given, not a single graphical representation of these short- or long-periodic changes are presented. We allow the number of data related to these periodic changes must cover a large span of time; and if regression of the line of nodes or advances of the line of apses are to be graphically seen, data covering 18.61 and 8.85 yr, respectively, are needed. In this work we particularly aim at the graphical representation of the periodic changes of the line of nodes. 相似文献
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