一种引力波天线的调谐方法

目前理论上预期的天体引力波源在低频段的引力辐射比较丰富[1-4].另一方面,目前使用的引力波天线绝大多数是机械共振天线,这类天线的Q值大都很高(104以上),频带甚窄(当v～10HZ时,Δv≤ 0.01Hz),在对某一特定的窄带引力辐射进行探测时很容易失调[5].因此,为了更好地探测引力波,并做到容易对准和跟踪它,自然希望天线具有比较低的共振频率和能够在一定的频率范围内方便地调谐. 作者曾在扭摆天线[6]的基础上研究了一种可调谐的引力波天线[7],指出这种天线容易在1—10Hz频率范围内调谐,这正是预期的天体物理过程所辐射的引力波的频谱峰值范围. …     

扭摆——探测低频引力波的一种可能的天线

本文研究了扭摆对引力波的响应和吸收截面,并对有关的问题进行了讨论,指出它可以作为探测低频引力波的机械共振天线。 关键词：     

集中质量音叉式引力波天线与Vela星引力辐射探测的探讨

本文提出并计算了一种接收Vela星引力辐射的集中质量音叉式机械谐振型低频天线。指出,由于Vela星引力波信号的连续性和单色性,可以采用信号积累方法提高接收灵敏度。最后给出了灵敏度可以达到目前理论估计的Vela星引力辐射强度的天线参数。此种天线也适用于其他低频引力波探测。 关键词：     

论引力波探测器方位与引力波源方位间的关系

本文从计算棒状引力波天线的指向性函数出发,讨论了引力波源的方位和天线棒方位之间的关系,找到了从符合实验数据求出引力波源方位以及利用单一引力波探测器对连续引力波源的定位方法。所得的结果也适用于其他形式的一维引力波天线。一旦引力波探测器的灵敏度达到足以确定引力波强度时,本文的结果无疑对引力波天文学将是很有意义的。 关键词：     

空间引力波探测计划-LISA系统设计要点

为了验证广义相对论,世界各国竞相开展了空间引力波探测方面的研究。本文以欧洲空间引力波探测LISA(Laser Interferometer Space Antenna)计划为例,根据基线设计,对LISA系统有效载荷及主要组件的设计进行了分析和阐述。LISA主要探测和研究低频引力波辐射,其工作频段为10^-3~1 Hz,工作距离为5×10⁶ km,预计能探测到双致密星系统以及星系合并引起的超大质量并合等波源,测距精度达到pm量级。以上研究希望能对我国未来的空间引力波探测计划有一定启示。     

用电磁方法探测高频引力波

 一、高频引力波不能使用传统方法进行探测根据广义相对论的预言,利用引力波的潮汐效应,可以对引力波进行探测。最早的引力波探测方法是共振质量法,其典型装置除韦伯棒(WeberBar)外,还有ALLEGRO(美国)、EXPLORER(意大利)等。它们的共同特点是将棒状或球状质量作为引力波的耦合天线,如果天线接收到了引力波信号,则天线上的不同部分之间将发生伸缩效应,利用声电转换(比如压电效应)可以将机械振动转换成电信号,测量电信号就可以确认是否探测到了引力波信号;这一类引力波探测装置对引力波共振的频率一般为102104Hz.     

在热噪声中的脉冲引力波的检测

一、引 言 探测引力波的原理,类似于接收电磁波.大家都知道带电粒子在电磁波的作用下会被激发而产生振动.一个质量块在引力波的作用下,它的各个质点也会产生“颤动”.从而使整个质量块产生机械形变.这种形变可以通过压电晶体等传感器转化为电信号后记录下来.但由于引力常数极为微小。引力波接收天线所接收到的引力波信号能量将大大低于天线的热噪声能量.而且根据理论上的预测,能够辐射强大引力波能量的天体活动过程是引力捕获和引力坍缩[1],这种过程是脉冲性的。前后持续仅几个毫秒,振动方向改变二到四次.现在采用的引力波接收天线一般都是…     

集中质量音叉式引力波天线的三自由度模型

本文将文献[1]提出的集中质量音叉式引力波天线的二自由度模型改进为三自由度模型,并给出了模型天线的实验结果。 关键词：     

光栅干涉集成麦克风研究

研制了一种光栅干涉集成麦克风，其传感核心尺寸为0.93 mm×0.34 mm×2.50 mm(体积小于0.8 mm³)，并且具有基于波长调谐实现控制工作点的功能。针对光栅干涉仪集成化设计问题，系统分析了激光器发散角对麦克风性能的影响。提出了集成型光栅干涉仪的设计指导，制作出了光栅干涉集成麦克风探头，探头整体尺寸为10.0 mm×10.0 mm×2.5 mm，并进行了实验测试。实验测试结果表明，该探头在50～300 Hz的低频范围内具有平坦的频率响应曲线，灵敏度为-33.11 dBV/Pa@251.2 Hz，在低频噪声监测领域有着广阔的应用前景。     

用于引力波关键技术验证的近地低成本商业卫星设计

地面引力波探测由于受到地表振动、重力梯度等噪声以及试验尺度的限制,探测频段被限制在10Hz以上,而对于更大特征质量和尺度的波源,探测频段主要在中低频段(0. 1 mHz～1 Hz)。因此,为避免地面干扰,需要在空间进行探测。由于引力波信号微弱,探测精度极高,针对空间引力波探测,国际上提出了以LISA为代表的空间引力波探测计划,国内中国科学院也提出了太极计划。然而,国内外的引力波探测卫星计划,对卫星的技术指标、设计复杂性和成本均提出了极高要求,短期之内难以实现。针对这一现实情况,本文参考LISA pathfinder的设计思路,设计一颗近地低成本商业卫星,针对引力波探测关键技术的验证需求,进行卫星任务需求分析及结构、热控、姿态控制等关键技术分析,提出商业化的低成本技术验证初步设想,希望能对空间引力波探测卫星总体设计提供一定借鉴。     

Gravitational free mass antenna as an angular gravity gradiometer

In the low frequency region 10⁻⁴–10⁻⁵ Hz a long base gravitational-wave interferometer is considered as a differential tiltmeter insensitive to perturbations of the local normal to the land. The effect of variations of the reciprocal deflection of two pendulum-mirrors is estimated for three conceivable scenarios of the earth core movements. The possibility of measurement of this effect is discussed according to the noise background estimate typical for modern gravitational antenna projects.     

Estimate of the cosmic ray background in an interferometric antenna for gravitational wave detection

The effect of the cosmic ray interaction in the masses of an interferometric antenna for gravitational wave (GW) detection is evaluated. In a 3 km antenna this background, mainly due to muons gives a limit, for 1 ms GW pulses, of h∼8.5×10^-23 with a frequency of 2×10^-1 events/year and 8.5×10^-26 with 4.1×10^-6 events/year. For GW having frequency>10 Hz the sensitivity limit is h∼1.7×10^-31. This background seems to allow unshielded operation of the interferometer test masses.     

Study of the Wind Characteristics of the Atmospheric Turbulence using a Multibeam Sodar

We present the results of acoustic sounding of the atmosphere in summer of 2001. The experiments were carried out using a multibeam bistatic sodar with two parabolic antennas of 15 m in diameter. The distance between the antennas was about 425 m. The transmitting acoustic antenna having 8^° beam width was pointed to the zenith. The four-beam operation of the receiving paraboloid was implemented by mounting four separate microphones in its focal plane. The width of each beam of the receiving antenna was 2.5^°. The beams of the transmitting and receiving antennas crossed at a height about 500 m. The sounding frequency was equal to 576 Hz. The acoustic-pulse duration and repetition period were 2 s and 8 s, respectively. A new procedure for experimental-data processing on the basis of analysis of temporary variations in the Doppler frequency shift of a scattered signal is proposed and approved. The approach based on using structural functions is applied. The preliminary results of analysis of one observation session are presented.     

Search for monochromatic sources with the GEOGRAV gravitational-wave antenna

Summary The data of 46 months of the GEOGRAV gravitational-wave antenna are analysed to search for monochromatic Doppler-shifted signals from rotating neutron stars, in the frequency band (856.2÷859.2) Hz. Two different methods were used. With the first, the gravitational radiation from the whole sky is investigated and a limit ofh≤1·10⁻²¹ is found. With the second method only the radiation from a single source is searched. The Galactic Centre and the Large Magellanic Cloud are considered as sources and the limit ofh≤6·10⁻²² is found.     

Initial operation at liquid-helium temperature of the M =2270 kg Al 5056 gravitational-wave antenna of the Rome group

Summary We report on the cooling at liquid-helium temperature of our 2270 kg 5056 Al bar at CERN. The liquid-helium container had been filled up to 1500 liters ensuring to keep the antenna cold for more than one month. The antenna is equipped with a resonant capacitive transducer operating at constant electrical charge with a FET low-noise amplifier. The transducer is tuned to the antenna within less than I Hz and the two normal-mode frequencies are ν₋=908.160 Hz and ν₊=924.234 Hz with an applied electrical field in the transducer of 10⁶ V/m. The corresponding overall merit factors areQ ₋=5.20·10⁶ andQ ₊=7.25·10⁶. The transducer has been tested up to an electrical field of 6·10⁶ V/m: in this condition we have βQ≈10⁴. The antenna has been in operation for several weeks giving, for the Brownian noise, values in agreement with the calculated values. We report also on the results of tests performed on a DC SQUID, whose input was connected to a commercial capacitor via a transformer with turn ratio of 1000. Supported in part by Japan Society for the Promotion of Science.     

Investigations of the near-millimeter-wave propagation on surface boundary layer path

Variations of the millimeter waves amplitude and angle-of-arrival caused by an influence of the atmospheric surface layer turbulence and striation were investigated on the 14-km propagation path, where radiotelescope RT-7.5 was used as a receiver antenna operating at the frequency of 90 GHz. In experiments, performed during two-year cycle, a set of statistical characteristics of the vertical and horizontal angle-of-arrival components were studied. Particularly, temporal spectra at the bandwidth 10^–5–10¹ Hz were obtained and an essential anisotropy of turbulence was found.     

Parametric Transducers for the Advanced Cryogenic Resonant-Mass Gravitational Wave Detectors

It is shown that a large improvement in liquid helium and ultra-cryogenically cooled resonant-mass gravitational wave detectors can be achieved through improved parametric transducers using either low loss sapphire dielectric resonators or niobium re-entrant cavities. Performance is analysed in relation to the existing resonant bar antenna Niobe and to massive spherical detectors. Applied to Niobe, a millisecond burst sensitivity of order 10^–20 can be achieved, corresponding to a spectral strain sensitivity of 2 × 10^-22 Hz with a 50 Hz bandwidth. Applied to an ultra-cryogenic 117 tonne spherical detector made from CuAl, a spectral strain sensitivity of better than 2 ×10^-23/ Hz with a bandwidth of order 100 Hz can be achieved, which is close to the quantum limit. This sensitivity is comparable to that of advanced interferometer detectors at this frequency.     

金原子团簇的分频散射光谱研究

液相金原子团簇是一种非线性光学介质.它在580nm处产生一个最强共振散射峰.当激发波长为290nm(1.03×10¹⁵Hz)时,液相金原子团簇在580nm(1/2×1.03×10¹⁵Hz)和870nm(1/3×1.03×10¹⁵Hz)分别产生一个1/2分频和1/3分频散射峰;当激发波长为580nm(5.02×10¹⁴Hz)时在290nm(2×5.02×10^-14Hz)和870nm(2/3×5.02×10¹⁴Hz)分别产生一个2倍频和2/3分频散射峰;当激发波长为870nm(3.34×10¹⁴Hz)时在580nm(3/2×3.34×10¹⁴Hz)和290nm(3×3.34×10¹⁴Hz)分别产生一个3/2分频和3倍频散射峰.分频散射和倍频散射峰与共振散射峰具有相似的散射行为.从激励光与液相金原子团簇相互作用的运动方程出发,根据傅氏变换理论,较好地解释了液相金原子团簇产生的一些非线性散射光谱.     

Development and test atT=4.2K of a capacitive resonant transducer for cryogenic gravitational-wave antennas

Summary The characteristics of a new capacitive resonant transducer developed and tested on a small (M=11.2 kg) cryogenic gravitational-wave antenna at the liquid helium temperature are presented. The resonator frequency can be tuned within 0.1 Hz of the antenna frequency. The system has a mechanical merit factorQ≃5·10⁵ and a ratio between the electrical energy in the transducer and the energy in the antenna β=3·10⁻³ atT=4.2 K. With these parameters, the transducer allows one to reach an effective noise temperatureT _eff≃60 mK using a cooled FET preamplifier, and, if coupled to a r.f.-SQUID, allows one to reachT _eff≃10 mK for the 5000 kg cryogenic gravitational-wave antenna of the Roma group at CERN (Geneva).

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Riassunto Si presentano le caratteristiche di un nuovo trasduttore risonante di tipo capacitivo. Il trasduttore è stato provato su una piccola antenna di 11.2 kg di massa, raffreddata alla temperature dell'elio liquido. La frequenza del risuonatore è stata accordata entro 0.1 Hz della frequenza dell'antenna. A 4.2 K, il sistema ha un fattore di merito meccanicoQ≃5·10⁵ ed il rapporto tra l'energia elettrica nel trasduttore e l'energia nell'antenna è β=3·10⁻³. Con i valori dei parametri ottenuti, il trasduttore permette di raggiungere una temperatura efficace di rumoreT _eff≃60 mK usando un amplificatore a FET raffreddato e, se accoppiato ad un r.f.-SQUID, consente di avereT _eff≃10 mK per l'antenna gravitazionale criogenica di 5000 kg del gruppo di Roma, in funzione presso il CERN (Ginevra).

     

Deformation of freshwater ice cover measured by a horizontal electric antenna

Electric fields arising in an ice cover as a result of deformation and interaction of ice slabs are measured on Lake Baikal. The features of the ice covering Lake Baikal are described. The frequency of the flexural vibrations of a floating ice sheet is calculated. For a square sheet with side a, the vibration frequency is f(Hz) = 222/a(m). It is found that ice cover vibrations cause the electric potential induced in a horizontal ungrounded antenna to oscillate with an amplitude of about 10 mV and a frequency of 1–13 Hz.