引力波与高频引力波探测

1、引力波与高频引力波探测,李芳昱 重庆大学物理系 China-VO 2009,ICGA9,2,Background and Motivation Coupling Electromagnetic Detection Scheme to High-Frequency Gravitational Waves Challenge and Opportunity,OUTLINE,3,Background,Classification of gravitational wave frequency bands. (1) 1Hz-104Hz, the detecting region by ground l

2、aser interferometer gravitational wave observatory, such as VIRGO, LIGO, etc. (2) 100Hz-103Hz, the detecting region by the resonant mass detectors, such as Weber Bar. (3) 10-4Hz-1Hz, the detecting region by Laser Interferometer Space Antenna, such as LISA. (4) 10-6Hz-10-3Hz, the detecting region by

3、ASTROD. (5) 107Hz-109Hz, the detecting region by electromagnetic microwave cavity or circular waveguide. (6) 108Hz-1011Hz, the detecting region by coupling systems of the microwave beams and static EM fields.,4,What are High-Frequency Gravitational Waves (HFGWs) ?,High Frequency Gravity Waves (HFGWs

4、) are gravitational waves (which differ from hydrodynamic gravity waves) that have frequencies of 100 kHz to 100 MHz (Hawking and Israel 1979). As their frequency increases, very high-frequency gravitational waves (VHFGWs) and ultra high-frequency gravitational waves (UHFGWs) are generated. These ha

5、ve frequencies of 100 MHz to 100 GHz and 100+ GHz, respectively. The generic term HFGWs describes all three of these bands. These waves move through the “fabric” of space similar to the way an ocean wave moves through the water. This “fabric,” as Einstein describes it, is called the “space-time cont

6、inuum” and is four-dimensional. It contains the usual three dimensions of space: for example, (1) east-west (2) north-south) (3) up down, but also includes the dimension of (4) time.,5,History of High-Frequency Gravitational Waves,Poincar, first mention of GWs, 1905 Robert L. Forward, lecture presen

7、ted at the Lockheed Astrodynamics Research Center in Bel-Air, California, USA, first mention of HFGWs, 1961 M. E. Gertsenshtein, 1962 L. Halpern and B. Laurent, relic HFGWs from Big Bang Richard Ingley, 2005, University of Birmingham, England,7,1 W.J.Kim et al., Phys.Rev.Lett. 96, (2006),2000402 2 M

8、.Giovannini, Phys.Rev.D 60, (1999),123511 M.Giovannini, Class.Quantum Grav. 16(1999),2905 3 M.Giovannini, Phys.Rev.D 73, (2006),083305 4 P.Chen astro-ph/0303350, (2003) 5 R.M.L.Baker,Jr., First International HFGW Conference, The MITRE Corporation, Paper HFGW-03-101. (2003) 6 L.P.Grishchuk, ibid, Pap

9、er HFGW-03-119. (2003) 7 G.V.Stephenson, ibid, Paper HFGW-03-104. (2003) 8 L.P.Grishchuk, gr-qc/0305051, gr-qc/0504018 9 A.M.Cruise, Class.Quantum Grav. 17(2000),2525 A.M.Cruise and R.M.J.Ingley, Class.Quantum rav.22(2005), s479. 10 A.Chincarini et al., First International HFGW Conference, The MITRE

10、 Corporation, Paper HFGW-03-103. (2003).,8,11 U.H.Gerlach, Phys.Rev.D 46, (1992),1239 12 W.K.Logi et al., Phys.Rev.D 16, (1977),2915 13 M. V. Mitskienich and A. I. Nesterov, Gen. Relativ Gravit. 27, 361 (1995). 14 F. Y. Li, M. X. Tang, and D. P. Shi, Phys. Rev. D 67, 104008 (2003) 15F.Y.Li, R.M.L. B

11、aker, Zhenyun Fang, G.V. Stephenson, Z.Y. Chen， Eur. Phys. J. C (2008) 56, 407423 (2008) 16 M. L. Tong, Y. Zhang, and F.Y. Li, Phys.Rev.D78, 024041 (2008) 17 F. Y. Li, M. X. Tang, and D. P. Shi, 2003 in High-Frequency Gravitational Wave Conference, the MITRE Corporation, Mclean, Virginia ,USA, Paper

12、 HFGW-03-108. 18 I. Osborne, et al Science 296, 1417 (2002). 19 C. Serife, Science 305, 464 (2004). 20 M. Livio and M. J. Rees, Science 309, 1022 (2005). 21 C. J. Hogan, American Scientist 90, 420 (2002). 22F. Y. Li, M. X. Tang, IJMPD 11, 1049(2002),9,23 G. Veneziano, Sci. Am. (Int. Ed.), 290, 30 (2

13、004). 24 G. S. B. Kogan and V. R. Rudenko, Class. Quantum Grav. 21, 3347 (2004). 25 M. Gasperini and G. Veneziano, Physics Reports 373, 1 (2003). 26 W. J. Wen, et al. Phys. Rev. Lett. 89, 223901 (2002). 27 L. Zhou, et al. Appl. Phys. Lett. 82, 1012 (2003). 28 W. J. Wen, Private communication, (2007)

14、. 29 P. Chen, Resonant Photon-Graviton Conversion in EM Fields: Form Earth to Heaven, Stanford Linear Accelerator Center-PUB-6666 (September, 1994) 30 D.I. Schuster, et al., cond-mat /0608639(2006). 31 K. Yamarnoto, et al., hep-ph /0101200(2001). 32 F. Y. Li, and R. M. L. Baker, Jr, In. Journal of M

15、odern Physics B 21, 3274 (2007) 33Li Jin, F.Y.Li, Y.H.Zhong, Chinese Physics B, 18, 3 0922 (2009),10,11,Why would we like to study this project?,According to the theory of general relativity, Gravitational waves (GWs) and Electromagnetic (EM) waves have a same propagating velocity in vacuum: Optimum

16、 coherence effect of the two fields may be generated The GHz (108Hz-1010Hz) are just typical microwave frequency band, one can use well-considered microwave technology in the frequency region. 109Hz-1010Hz are also typical frequencies of the HFGWs predicted by some laboratory schemes (e.g., Piezoele

17、ctric-Crystal-Resonator HFGW Generation),12,Characteristic dimensions of the EM detecting systems would be L1-10m, constructing cost will be greatly reduced. It is possible to use a series of new technology, such as superconductors, nanotechnology, high-quality factor microwave cavities, ultra-fast

18、science, strong field physics, cryogenic technology, ultra-high sensitivity microwave single photon detectors, and so on.,13,14,Some possible HFGW sources,15,16,17,Sharp Peak at 10 GHz,18,Birmingham University, Birmingham, England,19,Birmingham (Polarization) HFGW Detector(Differential Polarization

19、Angle of 10-40 Radians may Cause Measurable Femtosecond Time Difference),20,R. Ballantini et.al.,Institute of National Nuclear Physics, Genova, Italy,21,22,23,24,25,26,Geometry is key: X that is, the Standard Quantum Limit is so low (SQL 10-37, G. V. Stephenson STIF-2008) that a correctly-designed d

20、etector can have sufficient sensitivity to observe HFRGW of amplitude A 1030m/m,28,Resonant frequencies: 3-8GHz The power of the GB : p10-100w The spot radius : 5-8cm Background static magnetic field 3-5T Cryogenic condition T0.24k,29,30,31,The PPF and the BPF propagate along opposite directions in

21、the regions of 1st, 3rd,6th,and 8th octants, while they have the same propagating directions in the regions of 2nd, 4th , 5th and 7th octants.,32,33,34,35,The perturbative photon fluxes,36,Directional sensitivity of the system(hrms ),37,38,39,40,Constructing costs,41,42,美国高频引力波科学团队申报美国国家自然科学基金重点项目 申

22、报书首页摘要的中译本,美国国家自然科学基金项目申报书（草案）摘要 一种超高灵敏度的高频遗迹引力波探测系统 首席科学家， R.C.Woods教授，美国路易斯安娜州立大学 项目概要：申请方案的科学价值 这一申报项目需要得到美国科学界和产业界的支持，项目的目标是设计一种探测高频引力波的超高灵敏度的Li-Baker探测系统，联合研究的部门包括路易斯安娜州立大学和在加利福尼亚的输运科学公司。Li-Baker高频引力波探测系统拓展了爱因斯坦场方程的解，即发现了一种在一阶量级下引力波和光子的耦合效应，从而使得探测系统的灵敏度远高于目前已有的高频引力波探测方案。这一研究的成果将首先是高频引力波探测系统的前期工

23、程设计，并在基金持续资助下得以发展。这一探测系统的未来建设，将可以拓宽现有的激光干涉低频引力波天文台（注：美国现有两台低频引力波天文台，它们实际上是巨型迈克尔逊激光干涉仪，臂长为四公里。一台在路易斯安娜州，另一台在华盛顿州。他们的英文缩写为LIGO）的探测频道。上述Li-Baker探测系统将可望用于探测和展现高频遗迹引力波的宇宙背景辐射，并为澄清和阐明宇宙的起源作出贡献。这将致力于在一个全新的频带，作为首创并最有希望的去实现高频引力波的探测，这一频带大约在10GHz（1010Hz）左右，它已接近于在宇宙学范围产生的遗迹引力波的高频截止范围。同时，这一项目本身的信息、资料以及可交付的主要部分，将

24、是给美国国家自然科学基金委员会的一个最终报告。包括系列经过严格评审的学术刊物和权威的学术会议上发表的论文，以及系列IPR专利。 注：美国路易斯安娜州立大学是目前世界上唯一拥有低温质量谐振的低频引力波探测系统的科研院所，在这一领域拥有一批著名的物理学家和工程专家。,43,44,Challenge, issues and opportunity,Challenge and issues: How to generate a high-quality GB how to ensure a good cryogenic environment to suppress thermal noise how to further estimate and analyses the relevant noise sources how to ensure a good vacuum to avoid the scattering of photons and dielectric dissipation how to suppress possible leak EM fields from the cavities,45,how to make a best system combination to reduce and o