Water Cherenkov detectors:MILAGRO

This paper discusses the properties of using the water Cherenkov technique to detect air showers in the few hundred GeV to 100 TeV energy range. The responses of a 6 m² 2 m deep water Cherenkov counter and that of a 6 m² 10cm thick scintillator-lead sandwich counter to air shower electrons and photons is described. The advantages of water Cherenkov detector is outlined. Its application to do VHE gamma ray astronomy is discussed with particular reference to the MILAGRO telescope currently under construction. Milagro, a water-Cherenkov detector to do gamma ray astronomy above 100 Gev, uses an existing pool 60m × 80m by 8m, located in the Jemez mountains near Los Alamos, NM. The threshold of the MILAGRO detector is comparable to atmospheric Cherenkov detectors, however it has several advantages over these optical detectors. MILAGRO can operate 24 hours a day in all weather conditions and it has an open aperture which allows it to view the entire northern sky every day. These capabilities allow for a systematic all-sky survey to be done for the first time at these energies. MILAGRO will measure the Crab spectrum with high significance over a wide energy range, it will detect and measure the spectra from AGN's such as MRK 421 and it will search for short duration bursts from GRBs and possibly evaporating PBHs.     

正—反激组合式变换器与单端式变换器的比较

以５０Ｗ变换器为例，分别从磁性元件的大小，功率管上的电应力、磁恢复问题，输出纹波及输出特性等方面，详细分析比较了组合式变换器与单端式变换器的优缺点，并给出了具体数据，提出了正－反激组合式变换器具有电压应力低，磁性元件小，体积小，重量轻，输出纹波小及可靠性高的结论。     

镀膜光纤声光相位调制器频率响应特性的研究

本文对光纤声光相位调制器（OF—AOPM）的频率特性进行研究。分析了OF—AOPM的调相原理，研究结果表明：在调制频率远离氧化锌压电薄膜的半波谐振频率的时候，光相位的调制不仅依靠径向应力。同时还依靠轴向应力。通过同时考虑径向和轴向应力的变化，得出了OF—AOPM在整个频率域范围内的响应特性。     

谐振腔光纤陀螺频率调制原理及仿真

简述对谐振腔光纤陀螺入射光进行频率调制的基本方法，采用洛仑兹公式来描述光纤陀螺的传递函数，结合输入信号特征，建立其频域的数学模型，最后给出结果和相关仿真图形，以及关键参数的优化值和优化方向，再对全光路的结构提出具体的配置建议，仿真结果表明，谐振腔光纤陀螺具有良好的线性工作区间，精度也能够得到进一步的提高。     

1989年3月大宇宙线暴事件的特征

本文分析了1989年3月一系列大耀斑等离子体抛射引起的宇宙线强度变化的特征.除对中子成分分析外,还对μ介子成分及其各向异性特征作了分析,讨论了宇宙线强度变化与太阳耀斑特性和地磁扰动之间的关系。分析发现,宇宙线的Forbush下降不仅与太阳耀斑的级别、持续时间,以及在日面上的位置有关,而且还与光学耀斑是否伴有强的X射线暴、是否有强的射电爆发,以及是否引起强的地磁暴紧密有关.各向异性分析表明,3月大事件的各向异性明显小于宁静时的各向异性,这可能是因为受到太阳活动强烈调制之后,宇宙线各向异性趋于减小的原因.     

Real time localization of gamma ray bursts with INTEGRAL

The INTEGRAL satellite has been successfully launched in October 2002 and has recently started its operational phase. The INTEGRAL burst alert system (IBAS) will distribute in real time the coordinates of the gamma ray bursts (GRBs) detected with INTEGRAL. After a brief introduction on the INTEGRAL instruments, we describe the main IBAS characteristics and report on the initial results. During the initial performance and verification phase of the INTEGRAL mission, which lasted about two months, two GRBs have been localized with accuracy of 2–4 arcmin. These observations have allowed us to validate the IBAS software, which is now expected to provide quick (few seconds delay) and precise (few arcmin) localization for 10–15 GRBs per year.     

一种小功率逆变电源的设计及实现

介绍了一种小功率逆变电源电路的实现方法。对逆变主电路、电压控制电路、驱动电路、SCOTT电路进行了研究。该逆变电源具有工作可靠、波形失真小的特点。     

Low threshold particle arrays

While atmospheric Cherenkov telescopes have a small field of view and a small duty fraction, arrays of particle detectors on ground have a 1 sr field of view and a 100% duty fraction. On the other hand, particle detector arrays have a much higher energy threshold and an inferior hadron rejection as compared to Cherenkov telescopes. Low threshold particle detector arrays would have potential advantages over Cherenkov telescopes in the search for episodic or unexpected sources of gamma rays in the multi-TeV energy range. Ways to improve the threshold and hadron rejection of arrays are shown, based on existing technology for the timing method (with scintillator or water Cherenkov counters) and the tracking method (with tracking detectors). The performance that could be achieved is shown by examples for both methods. At mountain altitude (about 4000 m or above) an energy threshold close to 1 TeV could be achieved. For any significant reduction of the hadronic background by selecting muon-poor showers a muon detection area of at least 1000 m² is required, even for a compact array.     

Topological defects and highest energy cosmic and gamma rays

In this paper we review the hypothesis that a substantial part of the cosmic ray flux observed above about 10¹⁹ eV may be produced by decaying or annihilating topological defects left over from phase transitions in the early universe at grand unification energy scales ( 10¹⁶ GeV). Possible signatures of cosmic ray producing defect models are discussed which could be tested experimentally in the near future. We thereby focus on model independent universal spectral properties of the predicted particle fluxes.     

合成信号发生器参量的测量不确定度评定

对合成信号发生器测量结果的不确定度进行分析。