The detection of gravitational waves and the new era of multi-messenger astronomy
The detection of gravitational waves and the new era of multi-messenger astronomy
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引力波探测与多信使天文学新时代
DOI：
10.1007/s11433-016-5799-3
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发表时间：
2016-02
期刊：
影响因子：
--
通讯作者：
XiLong Fan
中科院分区：
文献类型：
--
作者：
XiLong Fan
引力波（GWs）是爱因斯坦1915年广义相对论（GR）的一个主要预测，引力波（GWs）首次被激光干涉仪引力波天文台（LIGO）的两个探测器直接探测到[1，图1，表1]。2015年9月14日，世界标准时间9点50分45秒，位于华盛顿州汉福德和洛杉矶利文斯顿的LIGO两台探测器探测到了巧合的GW事件（称为GW1509141）。通过将这一事件解释为起源于恒星质量黑洞（BHs）的碰撞，LSC和室女座协作星系（LVC）还报告了首次直接观测到双黑洞系统合并形成单个黑洞[1]。1916年，阿尔伯特·爱因斯坦通过求解线性化的弱引力场爱因斯坦方程，首次得到了gww是以光速传播的空间应变横波。这些波的观测证据首先是从双星脉冲星系统PSR B1913+ 16的轨道能量损失中获得的。另一方面，黑洞首先是作为真空爱因斯坦方程的精确解得到的，首先是由史瓦西在静态球对称情况下得到的，然后是由克尔在静态轴对称情况下得到的。直到很久以后，人们才开始认识到这些解决方案的物理意义，即黑洞。数学研究建立了所谓的无毛定理，该定理指出黑洞的特征仅在于它们的质量、自旋和电荷。黑洞微扰理论的发展表明黑洞应该是稳定的，并且可能是引力坍缩的终点。还得到了坍缩恒星和碰撞黑洞时空的微扰解和全数值解。虽然已经通过电磁（EM）观测确定了强有力的黑洞候选者，并通过人口综合理论和坍缩和合并的数值模拟进行了预测，但黑洞附近的时空结构从未被探测过。GW探测实验始于20世纪60年代韦伯的共振质量探测器，随后是共振探测器的国际网络。后来人们意识到，大型激光干涉仪GW探测器应该在更宽的频率范围内具有更好的灵敏度。自20世纪90年代以来，包括LIGO、VIRGO、GEO 600、TAMA 300在内的此类探测器的国际网络已经建立并运行。从2002年到2009年，第一代探测器进行了一系列的操作，但没有做出积极的检测。先进的LIGO探测器[2]刚刚完成了第一次观测运行（O1），而先进的VIRGO正在调试中。日本新建造的引力波探测器KAGRA可能会在2017年开始运行。这些探测器使用具有正交臂的迈克尔逊干涉仪和镜面赋予的测试质量来测量GWs，这可以被视为诱导其臂长的差异变化。为了观测非常微弱的GWs，先进的LIGO探测器对基本的4公里长度的迈克尔逊干涉仪进行了一些改进，以最大限度地减少照片噪声的影响，并且还采用/开发了新的方法和技术，用于测试质量的悬挂系统和材料及其悬挂，以减少地震噪声和热噪声，以及用于减少地面运动影响的控制系统（详见参考文献[2]）。两个探测器名义运行，在GW150914观测时间内输出校准良好[2-4]。
For the first time, gravitational waves (GWs), a major prediction of Einstein’s 1915 general theory of relativity (GR), has been detected directly by the two detectors of the Laser Interferometer Gravitational-Wave Observatory (LIGO)[1, Figure 1, Table 1]. On September 14, 2015 at 09: 50: 45 UTC two detectors from LIGO, located at LIGO Hanford, WA, and Livingston, LA sites, detected the coincidental GW event (referred to as GW1509141)). By interpreting the event as having originated from colliding stellar-mass black holes (BHs), the LSC and Virgo collaborations (LVC) also reported the first direct observation of a binary BH system merging to form a single BH [1]. As first obtained by Albert Einstein in 1916, by solving the linearized Einstein’s Equations which are valid for weak gravitational fields, GWs are transverse waves of spatial strain that travel at the speed of light. Observational evidence for these waves was first obtained from the loss in orbital energy of the binary pulsar system PSR B1913+ 16. BHs on the other hand, were first obtained as exact solutions to the vacuum Einstein’s equations, first by Schwarzschild in the static, spherically symmetric case, and then by Kerr in the stationary, axisymmetric case. It was not until much later that people started appreciating the physical significance of these solutions, as BHs. Mathematical studies established the so-called no-hair theorems, which state that BHs are only characterized by their mass, spin and electric charge. The development of BH perturbation theory indicated that BH should be stable, and are plausible end points of gravitational collapse. Perturbative and fully numerical solutions for space-times of collapsing stars and colliding BHs have also been obtained.While strong candidates of BHs have been identified through electromagnetic (EM) observations and predicted from population synthesis theories and numerical simulations of collapses and mergers, space-time structures near black holes have never been probed. GW detection experiments began with Weber’s resonant mass detectors in the 1960s, followed by an international network of resonant detectors. It was later realized that large-scale, laser interferometer GW detectors should have much better sensitivity, over a much broader frequency range. Since the 1990s, an international network of such detectors, including LIGO, VIRGO, GEO 600, TAMA 300, have been built and operated. From 2002 to 2009, a series of operations have been undertaken by the first-generation detectors, without making a positive detection. Advanced LIGO detectors [2] have just completed its first Observation Run (O1), while Advanced VIRGO is in commissioning. KAGRA, the newly constructed Japanese gravitational-wave detector, may start operation in 2017. These detectors use Michelson interferometers with orthogonal arms and mirror-endowed test masses to measure GWs, which could be seen as inducing differential changes in their arm lengths. To observe the remarkably weak GWs, Advanced LIGO detectors have several enhancements to the basic 4 km length Michelson interferometers for minimizing the impact of photo shot noise, and also adopt/develop novel approaches and technique on suspension system and materials in the test masses and their suspensions for reducing the seismic noise and thermal noise, as well as on control systems for reducing the impact of ground motions (see detail in ref.[2]). Two detectors were operating nominally, and their outputs are well calibrated during the GW150914 observation time [2-4].
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DOI：
10.1007/s11433-015-5748-6
发表时间：
2015-12
期刊：
Science China Physics, Mechanics & Astronomy
影响因子：
--
作者：
D. Blair;L. Ju;Chunnong Zhao;L. Wen;Q. Chu;Q. Fang;R. Cai;Jiangrui Gao;Xuechun Lin;
通讯作者：
D. Blair;L. Ju;Chunnong Zhao;L. Wen;Q. Chu;Q. Fang;R. Cai;Jiangrui Gao;Xuechun Lin;
影响因子：
2.1
作者：
Duncan A. Brown;K. Vahi;M. Taufer;Von Welch;E. Deelman;Lorena A. Barba;George K. Thiruvathukal
通讯作者：
Duncan A. Brown;K. Vahi;M. Taufer;Von Welch;E. Deelman;Lorena A. Barba;George K. Thiruvathukal
DOI：
10.1007/s11433-015-5738-8
发表时间：
2015-12
期刊：
Science China Physics, Mechanics & Astronomy
影响因子：
--
作者：
V. Mitrofanov;S. Chao;H. Pan;L. Kuo;G. Cole;J. Degallaix;B. Willke
通讯作者：
V. Mitrofanov;S. Chao;H. Pan;L. Kuo;G. Cole;J. Degallaix;B. Willke
DOI：
--
发表时间：
2015-09
期刊：
Journal of materials chemistry. B
影响因子：
--
作者：
Xingjiang Zhu;L. Wen;G. Hobbs;R. Manchester;R. Shannon
通讯作者：
Xingjiang Zhu;L. Wen;G. Hobbs;R. Manchester;R. Shannon
下一代引力波天文学探测器
DOI：
10.1007/s11433-015-5747-7
发表时间：
2015-12
期刊：
Science China Physics,Mechanics & Astonomy
影响因子：
--
作者：
Blair David;Ju Li;Zhao ChunNong;Wen LinQing;Miao Haixing;Cai RongGen;Gao JiangRui;Lin XueChun;Liu Dong;Wu Ling-An;Zhu ZongHong;Hammond Giles;Paik Ho Jung;Fafone Viviana;Rocchi Alessio;Blair Carl;Ma YiQiu;Qin JiaYi;Page Michael
通讯作者：
Page Michael