共查询到18条相似文献，搜索用时 156 毫秒
1.
2.
龚雪飞 徐生年 袁业飞 白姗 边星 曹周键 陈葛锐 董鹏 高天舒 高伟 黄双林 李玉龙 刘影 罗子人 邵明学 孙宝三 唐文林 于品 徐鹏 臧云龙 张海鹏 刘润球 《天文学进展》2015,(1):59-83
空间引力波探测是研究宇宙早期恒星演化和星系形成、黑洞和星系的共同成长等天文学和宇宙学重大问题的一条重要可能途径。经过两期科学院先导科技专项空间科学预研究课题的开展,通过权衡技术的可行性与科学的前瞻性,选择以高红移开始的中至大质量双黑洞并合系统、星团等稠密动力学环境中涉及中等质量黑洞的双黑洞引力波波源为主要科学目标,给出了我国毫赫兹至赫兹频段空间引力波探测任务计划的初步设计。以该任务设计建议为依据,简要介绍空间引力波探测及其作为一种新的天文观测手段的科学内涵,以及我国空间引力波探测任务设计的科学目标和探测潜力。 相似文献
3.
引力波是爱因斯坦和其他物理学家提出的关于广义相对论的四大预言之一。除了PSR1 91 3 + 1 6引力辐射阻尼的观测提供了引力波存在的间接证据外 ,科学家至今仍没有在实验室中确证引力波的存在。由于人类目前的技术水平还不可能在实验室中产生强度可供探测的引力波 ,而宇宙中存在大量大质量、高速运动的天体 ,有可能产生较强的引力波 ,天体引力波源自然成为现阶段科学家研究引力波的首选。本文介绍广义相对论框架下预言的引力波性质 ,引力波探测的理论依据 ,共振型棒式天线和激光干涉仪两大类探测器的基本原理 ,引力波探测实验的现状和面临的困难 ,科学家采取的对策 ,以及爆发型和连续型两类天体引力波源。最后介绍了正在计划中的几个引力波探测空间实验 相似文献
4.
引力波、引力波源和引力波探测实验 总被引：1，自引：0，他引：1
引力波是爱因斯坦和其他物理学家提出的关于广义相对论的四大预言之一。除了PSR1913＋16引力辐射阻尼的观测提供了引力波存在的间接证据外，科学家至今仍没有在实验室中确证引力波的存在。由于人类目前的技术水平还不可能在实验室中产生强度可供探测的引力波，而宇宙中存在大量大质量，高速运动的天体，有可能产生较强的引力波，天体引力波源自然成为现阶段科学家研究引力波的首选。本文介绍广义相对论框架下预言的引力波性质，引力波探测的理论依据，共振型棒式天线和激光干涉仪两大类探测器的基本原理，引力波探测实验的现状和面临的困难，科学家采取的对策，以及爆发型和连续型两类天体引力波源。最后介绍了正在计划中的几个引力波探测空间实验。 相似文献
5.
引力波和引力波望远镜的发展 总被引：2，自引：1，他引：1
简要回顾了广义相对论中相关的引力波理论，讨论了对引力波进行探测的重要意义和几种可能的途径；系统介绍了近50年来国际上对引力波进行探测的主要活动，以及当前几个具有代表性的引力波望远镜工程的进展。 相似文献
6.
2015年9月14日,美国激光干涉引力波天文台(LIGO)捕捉到了距离地球13亿光年外的一对双黑洞并合产生的引力波信号(GW150914)。经过长达数月的数据分析,LIGO团队确证了激光干涉仪在该引力波信号穿过时产生的大约是一亿亿分之一厘米尺度的振荡变化,并于2016年2月11日对外公布了这项惊人发现。这是人类首次直接探测到爱因斯坦广义相对论预言的引力波信号,并证实了双黑洞的存在。引力波探测器为探测宇宙提供了不同于电磁波(光)的全新方法,现在我们不仅能用望远镜“看”缤纷多彩的宇宙,还能用引力波探测器“听”波澜壮阔的宇宙。2017年的诺贝尔物理学奖也因此颁给了对引力波探测作出杰出贡献的三位物理学家:雷纳·韦斯(Rainer Weiss)、基普·索恩(Kip Stephen Thorne)和巴里·巴里什(Barry Clark Barish)。 相似文献
7.
8.
引力波是广义相对论的重要推论之一,迄今为止尚未被直接探测到。上世纪末共振棒引力波探测网曾联合运行.历经十余年的努力,世界激光干涉引力波探测网已经初步形成。今后一、两年将会同步运行。最新的关于中子双星的天文观测和分析给引力波探测带来了希望。 相似文献
9.
类星体OJ 287的研究已经有100多年的历史,它呈现周期性双峰爆发现象,爆发周期为12 yr,比较好地解释观测的模型是双黑洞模型,即次黑洞绕主黑洞运动,并撞击主黑洞吸积盘从而引起爆发.此模型合理地解释了OJ 287的光变曲线并正确预言了未来爆发时间,这间接证明了广义相对论进动效应以及引力波的存在.星系中心大质量黑洞是一类重要的引力波源,而精确确定了其内部组分运动学方程的星系非常少,由于双黑洞模型提供了精确的黑洞运动轨道,故可以在这个运动轨道基础上研究其引力波辐射.在已有工作基础上,采用后牛顿近似方法首次得到了引力波辐射功率和波形随时间的演化关系,根据目前引力波探测设备IPTA(International Pulsar Timing Array)的进展情况,未来十几年内对OJ 287的引力波直接探测将成为可能. 相似文献
10.
《天文学进展》2014,(3)
引力波的存在是爱因斯坦在广义相对论中提出的一个重要预言,引力波探测是当代物理学最重要的前沿领域之一。经过近半个世纪的艰苦努力,随着几个大型激光干涉仪引力波探测器在21世纪初的出现并于近几年达到前所未有的灵敏度,引力波探测进入了一个崭新的时代。人类有望在第二代地基激光干涉仪引力波探测器开始科学运行(约2015年)之后的几年内,不仅可以直接探测到引力波,更将打开一扇观测宇宙的新窗口。引力波探测也将成为继电磁辐射、宇宙线和中微子之后,人类探索宇宙奥秘的又一重要手段。介绍了激光干涉仪引力波探测器的性能和工作原理,详细分析了其关键部件,如:迈克尔孙干涉仪、法布里–珀罗腔、功率循环系统、激光器、清模器、倒摆、单体几何反弹簧过滤器、真空系统等的结构、性能和工艺特点,展望了其广阔的发展前景。 相似文献
11.
D. M. Sedrakian M. Benacquista K. M. Shahabassian A. A. Sadoyan M. V. Hairapetyan 《Astrophysics》2003,46(4):445-454
Undamped quasiradial fluctuations of rotating neutron stars and the gravitation radiation generated by them are discussed. Two possible sources of energy for maintaining these fluctuations are mentioned: the energy of deformation of the decelerating neutron star (spin down) and the energy released during a jump in the star's angular velocity (glitch). Expressions are derived for the intensity of the gravitational radiation and the amplitude of a plane gravitational wave for an earthbound observer. Estimates of these quantities are obtained for the Vela and Crab pulsars, for which the secular variation in the angular velocity is most often accompanied by irregular variations. It is shown that gravitational waves from these pulsars could be detected by the new generation of detectors. 相似文献
12.
The state of supranuclear matter in compact stars remains puzzling, and it is argued that pulsars could be strangeon stars. What would happen if binary strangeon stars merge? This kind of merger could result in the formation of a hyper-massive strangeon star, accompanied by bursts of gravitational waves and electromagnetic radiation(and even a strangeon kilonova explained in the paper). The tidal polarizability of binary strangeon stars is different from that of binary neutron stars, because a strangeon star is self-bound on the surface by the fundamental strong force while a neutron star by the gravity, and their equations of state are different. Our calculation shows that the tidal polarizability of merging binary strangeon stars is favored by GW170817. Three kinds of kilonovae(i.e., of neutron, quark and strangeon) are discussed, and the light curve of the kilonova AT 2017 gfo following GW170817 could be explained by considering the decaying strangeon nuggets and remnant star spin-down. Additionally,the energy ejected to the fireball around the nascent remnant strangeon star, being manifested as a gamma-ray burst, is calculated. It is found that, after a prompt burst, an X-ray plateau could follow in a timescale of 10~2-10~3 s. Certainly, the results could be tested also by further observational synergies between gravitational wave detectors(e.g., Advanced LIGO) and X-ray telescopes(e.g., the Chinese HXMT satellite and e XTP mission), and especially if the detected gravitational wave form is checked by peculiar equations of state provided by the numerical relativistical simulation. 相似文献
13.
Zhao Wen Zhang Xing Liu Xiao-jin Zhang Yang Wang Yun-yong Zhang Fan Zhao Yu-hang Guo Yue-fan Chen Yi-kang Ai Shun-ke Zhu Zong-hong Wang Xiao-ge Lebigot Eric Du Zhi-hui Cao Jun-wei Qian Jin Yin Cong Wang Jian-bo Wen Lin-qing 《Chinese Astronomy and Astrophysics》2018,42(4):487-526
The recent discovery of gravitational-wave burst GW150914 marks the coming of a new era of gravitational-wave astronomy, which provides a new window to study the physics of strong gravitational field, extremely massive stars, extremely high energy processes, and extremely early universe. In this article, we introduce the basic characters of gravitational waves in the Einstein's general relativity, their observational effects and main generation mechanisms, including the rotation of neutron stars, evolution of binary systems, and spontaneous generation in the inflation universe. Different sources produce the gravitational waves at quite different frequencies, which can be detected by different methods. In the lowest frequency range (f < 10?15 Hz), the detection is mainly dependent of the observation of B-mode polarization of cosmic microwave background radiation. In the middle frequency range (10?9 < f < 10?6 Hz), the gravitational waves are detected by analyzing the timing residuals of millisecond pulsars. And in the high frequency range (10 ? 4 < f < 104 Hz), they can be detected by the space-based and ground-based laser interferometers. In particular, we focus on the main features, detection methods, detection status, and the future prospects for several important sources, including the continuous sources (e.g., the spinning neutron stars, and stable binary systems), the burst sources (e.g., the supernovae, and the merge of binary system), and the stochastic backgrounds generated by the astrophysical and cosmological process. In addition, we forecast the potential breakthroughs in gravitational-wave astronomy in the near future, and the Chinese projects which might involve in these discoveries. 相似文献
14.
V. Pierro I.M. Pinto A.D. Spallicci E. Laserra F. Recano 《Monthly notices of the Royal Astronomical Society》2001,325(1):358-372
The relevance of orbital eccentricity in the detection of gravitational radiation from (steady state) binary stars is emphasized. Computationally effective (fast and accurate) tools for constructing gravitational wave templates from binary stars with any orbital eccentricity are introduced including tight estimation criteria of the pertinent truncation and approximation errors. 相似文献
15.
Gravitational wave detection through microlensing? 总被引：1，自引：0，他引：1
Roberto Ragazzoni Gianpaolo Valente Enrico Marchetti 《Monthly notices of the Royal Astronomical Society》2003,345(1):100-110
It is shown that accurate photometric observations of a relatively high-magnification microlensing event ( A ≫ 1) , occurring close to the line of sight of a gravitational wave (GW) source, represented by a binary star, can allow the detection of subtle gravitational effects. After reviewing the physical nature of such effects, it is discussed to what extent these phenomena can actually be caused by GWs. Expressions for the amplitude of the phenomena and the detection probability are supplied. 相似文献
16.
V. S. Imshennik 《Astronomy Letters》2008,34(6):375-388
We consider the evolution of a neutron star binary system under the effect of two factors: gravitational radiation and mass transfer between the components. Gravitational radiation is specified under the justified assumption of a circular orbit and point masses and in the approximation of a weak gravitational field at nonrelativistic velocities of the binary components. During the first evolutionary phase determined only by gravitational radiation, the neutron stars approach each other according to a simple analytical solution. The second evolutionary phase begins at the time of Roche-lobe filling by the low-mass component, when the second factor, mass transfer as a result of mass loss by the latter, also begins to affect the evolution. Under the simplest assumptions of conservative mass transfer and exact equality between the Roche-lobe radius and the radius of the low-mass neutron star, it is still possible to extend the analytical solution of the problem of evolution to its second phase. We present this complete solution at both phases and, in particular, give theoretical light curves of gravitational radiation that depend only on two dimensionless parameters (m t and δ 0). Based on the solution found, we analyze the theoretical gravitational signals from SN 1987A; this analysis includes the hypothesis about the rotational explosion mechanism for collapsing supernovae. 相似文献
17.
Gravitational waves from mergers of black holes and neutron stars are now being detected by LIGO. Here we look at a new source of gravitational waves, i.e., a class of dark matter objects whose properties were earlier elaborated. We show that the frequency of gravitational waves and strains on the detectors from such objects (including their mergers) could be within the sensitivity range of LIGO. The gravitational waves from the possible mergers of these dark matter objects will be different from those produced by neutron star mergers in the sense that they will not be accompanied by electromagnetic radiation since dark matter does not couple with radiation.
相似文献18.
《New Astronomy》2016
Gravitational wave bursts in the formation of neutron stars and black holes in energetic core-collapse supernovae (CC-SNe) are of potential interest to LIGO-Virgo and KAGRA. Events nearby are readily discovered using moderately sized telescopes. CC-SNe are competitive with mergers of neutron stars and black holes, if the fraction producing an energetic output in gravitational waves exceeds about 1%. This opportunity motivates the design of a novel Sejong University Core-CollapsE Supernova Survey (SUCCESS), to provide triggers for follow-up searches for gravitational waves. It is based on the 76 cm Sejong university telescope (SUT) for weekly monitoring of nearby star-forming galaxies, i.e., M51, M81-M82 and blue dwarf galaxies from the unified nearby galaxy catalog with an expected yield of a few hundred per year. Optical light curves will be resolved for the true time-of-onset for probes of gravitational waves by broadband time-sliced matched filtering. 相似文献