微波偶极子在生物介质中比吸收率分布研究

微波偶极子辐射器在生物介质中比吸收率（ＳＡＲ）分布研究对脓道肿瘤热疗有重要实用意义,本文根据电磁场理论模型和迭加原理,采用高斯积分法和辛普森积分法相结合,分别计算了无水冷、有水冷,单缝隙和双缝隙微波偶极子辐射器在生物介质中的ＳＡＲ分布,结果表明,水冷可以较好地改善ＳＡＲ径向分布,增加治疗深度;而双缝隙可比单缝隙具有更为均匀的轴和ＳＡＲ分布,增加治疗体积,该研究结果可为腔道水冷式微波偶极子辐射器的研     

微波偶极子在生物介质中比吸收率分布研究

微波偶极子辐射器在生物介质中比吸收率（ＳＡＲ）分布研究对腔道肿瘤热疗有重要实用意义本文根据电磁场理论模型和迭加原理,采用高斯积分法和辛普森积分法相结合,分别计算了无水冷、有水冷、单缝隙和双缝隙微波偶极子辐射器在生物介质中的ＳＡＲ分布结果表明：水冷可以较好地改善ＳＡＲ径向分布,增加治疗深度;而双缝隙可比单缝隙具有更为均匀的轴向ＳＡＲ分布,增加治疗体积该研究结果可为腔道水冷式微波偶极子辐射器的研制设计和临床应用提供参考依据     

FR^A—模型成的格

研究了全体ＦＲ＾Ａ－模型成的格ＦＲ＾Ａ（Ｍ）及其子格的结构，证得ＦＲ＾Ａ（Ｍ）及其子格为模格。利用同态理论研究同态模间形成的ＦＲ＾Ａ－模格的相互关系，得到一些重要的同态与同构定理。最后指出ＦＲ＾Ａ（Ｍ）不是配格。     

全反式维甲酸对人真皮成纤维细胞RXR的表达影响

Ｎｏｒｔｈｅｒｎ杂交检测人真皮成纤维细胞维甲类Ｘ受体（ＲＸＲ）的表达。结果显示,细胞中只有ＲＸＲα和β的信息ＲＮＡ表达,无γ受体信息ＲＮＡ表达;用全反式维甲酸（ＡＴ－ＲＡ）刺激细胞于不同时段,对ＲＸＲ家族无诱导作用。表明人真皮成纤维细胞ＲＸＲ基因家族的表达调节完全不同于ＲＡＲ基因家族     

微波（2450MHz）对整体小白鼠红细胞膜的损伤效应及药物防护

本文采用２４５０ＭＨｚ微波慢性辐射整体昆明小白鼠，从分子水平研究微波对小白鼠红细胞膜的影响。选择功率密度０ｍＷ／ｃｍ２、５ｍＷ／ｃｍ２（ＳＡＲ＝５．５ｍＷ／ｇ）、１０ｍＷ／ｃｍ２（ＳＡＲ＝１１ｍＷ／ｇ）的微波连续辐射小白鼠４０天，每天６小时。发现１０ｍＷ／ｃｍ２的微波对小白鼠红细胞膜的损伤较为明显。表现为小白鼠红细胞的渗透脆性增加，膜脂流动性下降，血浆丙二醛（ＭＤＡ）及红细胞膜ＭＤＡ均为明显升高，但红细胞溶血度未增加，红细胞ＳＯＤ、红细胞膜ＡｃｈＥ活动和膜蛋白组份的百分含量也未见明显变化。此外，本文还从自由基角度初步探讨了微波辐射损伤的机理。实验表明，喂服维生素Ｃ的小白鼠有抗微波损伤的作用，这启示一定剂量的维生素Ｃ对微波损伤有防护作用。     

渔船冷冻保鲜方法的探讨

渔船冷冻保鲜方法的探讨ＯＮＭＥＴＨＯＤＯＦＦＲＥＥＺＩＮＧＡＮＤＳＴＯＲＡＧＥＯＮＦＩＳＨＩＮＧＶＥＳＳＥＬＳ宋协法ＳｏｎｇＸｉｅｆａ（青岛海洋大学水产学院，青岛２６６００３）（ＯｃｅａｎＵｎｉｖｅｒｓｉｔｙｏｆＱｉｎｇｄａｏ，Ｑｉｎｇｄａｏ２６６０...     

中国人重症肌无力的遗传易感性研究

重症肌无力与ＨＬＡⅡ类基因关联性在不同人种和民族中具有不同遗传易感性。为探讨中国人重症肌无力（ＭＧ）与ＨＬＡ－ＤＱ分子关联性，采用聚合酶链式反应—限制性片段长度多态性（ＰＣＲ－ＲＦＬＰ）方法，分析了５０例中国正常人及４９例重症肌无力患者的ＨＬＡ－ＤＱＡ１和－ＤＱＢ１座位的基因型。结果：共检出正常人ＤＱＡ１等位基因８种，ＤＱＢ１等位基因１０种，重症肌无力患者ＤＱＡ１等位基因８种，ＤＱＢ１等位基因９种。结果分析表明ＤＱＡ１＊０５０１与ＭＧ成负相关，ＤＱＢ１＊０３０２与ＭＧ成正相关。从基因水平首次用ＰＣＲ－ＲＦＬＰ方法得出中国人重症肌无力ＤＱ分子的易感基因型。     

人胰岛素原类似物（B—Arg—Arg—A）基因的构建和表达

用聚合酶链反应（ＰＣＲ）法将Ｃ肽为６个氨基酸残基的胰岛素原类似物基因删除突变成Ｃ肽仅为２个精氨酸残基的胰岛类原类似物基因，即把ＰＵＣ１８ＢＣ＇Ａ改建为ＰＵＣ１８ＢＲ２Ａ。再将ＰＵＣ１８ＢＲ２Ａ与ＰＪＧ１０５且为表达质粒ＰＪＧ１０７，使Ｂ－Ａ－Ａ与ＰＪＧ１０５编码的一种多肽成融合蛋白在大肠杆菌体系中表达。融合蛋白占细菌蛋白总量的５８％。表达产物具有人胰岛素放射免疫活性。     

交叉指电容的计算机辅助设计

本文用矩量法（ＭＯＭ）准确分析了单片微波集成电路（ＭＭＩＣ）中一种常用电容元件──交叉指电容（ＩＮＴＥＲＤＩＧＩＴＡＬＣＡＰＡＣＩＴＯＲ）的静态电容矩阵之后，再利用耦合微带线（阵）理论计算了其等效电感和损耗电阻，从而得到其Ｓ参数，经文献验证和实验验证，所得结果准确。     

微波处理对几种蔬菜种子萌发的影响(简报)

微波处理对几种蔬菜种子萌发的影响（简报）周丽艳马英华＊（河北农业技术师范学院农学系，昌黎，０６６６００）ＴＨＥＩＮＦＬＵＥＮＣＥＯＦＭＩＣＲＯ－ＲＡＹＯＮＴＨＥＧＥＲＭＩＮＡＴＩＯＮＯＦＶＥＧＥＴＡＢＬＥＳＥＥＤＳ（ＢＵＬＬＥＴＩＮ）ＺｈｏｕＬｉｙａ...     

太阳射电微波爆发谱与HXR的统计研究

The statistics analysis is carried out for some coincident event data on solar microwave bursts and HXR bursts. Some significant results and reasonable proposition are presented.     

用电流环结合模型解释微波爆发中的FS现象

利用Tajima和Sakai提出的解释太阳耀斑现象的电流环结合模型,分析了短厘米波段微波爆发中的精细结构现象.结果表明,观测事实是对这一新的理论模型的有力支持.     

High-velocity streams of dust originating from Saturn

High-velocity submicrometre-sized dust particles expelled from the jovian system have been identified by dust detectors on board several spacecraft. On the basis of periodicities in the dust impact rate, Jupiter's moon Io was found to be the dominant source of the streams. The grains become positively charged within the plasma environment of Jupiter's magnetosphere, and gain energy from its co-rotational electric field. Outside the magnetosphere, the dynamics of the grains are governed by the interaction with the interplanetary magnetic field that eventually forms the streams. A similar process was suggested for Saturn. Here we report the discovery by the Cassini spacecraft of bursts of high-velocity dust particles (> or = 100 km s(-1)) within approximately 70 million kilometres of Saturn. Most of the particles detected at large distances appear to originate from the outskirts of Saturn's outermost main ring. All bursts of dust impacts detected within 150 Saturn radii are characterized by impact directions markedly different from those measured between the bursts, and they clearly coincide with the spacecraft's traversals through streams of compressed solar wind.     

New developments of MSRT’s working modes: One-dimensional radio heliograph and IPS telescope

This note introduces the newly developed working modes, i.e. one-dimensional meter-wave radio heliograph (MRH) and interplanetary scintillation (IPS) telescope, of meter-wave aperture synthesis radio telescope (MSRT) at Beijing Astronomical Observatory (BAO). The note describes briefly the scientific objectives, configurations of the hardware and software, and functions of the system. It presents the examples of observations on solar meter-wave bursts and IPS with the two new working modes. The results indicated that new modes not only can provide the information on the evolution of solar activities with space and time, but also can trace and monitor the propagation and spatial distribution of interplanetary plasma shock resulting from solar activities and the instability of the ionosphere, etc. Both modes are new facilities that could fill the gaps in scientific frontiers.     

Swift/BAT伽玛暴的经验谱能关系

我们选取76个红移已知Swift伽玛暴(含有61个长暴和15个短暴),分析了各向同性能量,光度和峰值能量之间的相关性,研究发现Swift长暴存在Amati关系,而短暴存在Ghirlanda关系和Amati关系。我们还发现了Swift/BAT长暴和短暴的Ep.i-Lp关系都分别存在且是一致的,并且符合Zhang,DaiHuang之前利用多个卫星数据得到的结果。     

The formation of the first low-mass stars from gas with low carbon and oxygen abundances

The first stars in the Universe are predicted to have been much more massive than the Sun. Gravitational condensation, accompanied by cooling of the primordial gas via molecular hydrogen, yields a minimum fragmentation scale of a few hundred solar masses. Numerical simulations indicate that once a gas clump acquires this mass it undergoes a slow, quasi-hydrostatic contraction without further fragmentation; lower-mass stars cannot form. Here we show that as soon as the primordial gas--left over from the Big Bang--is enriched by elements ejected from supernovae to a carbon or oxygen abundance as small as approximately 0.01-0.1 per cent of that found in the Sun, cooling by singly ionized carbon or neutral oxygen can lead to the formation of low-mass stars by allowing cloud fragmentation to smaller clumps. This mechanism naturally accommodates the recent discovery of solar-mass stars with unusually low iron abundances (10(-5.3) solar) but with relatively high (10(-1.3) solar) carbon abundance. The critical abundances that we derive can be used to identify those metal-poor stars in our Galaxy with elemental patterns imprinted by the first supernovae. We also find that the minimum stellar mass at early epochs is partially regulated by the temperature of the cosmic microwave background.     

On theories of solar type III radio bursts

In solar radiophysics,many theories for type Ⅲ bursts have been proposed during the past 60 years.Almost all these theories are based on the plasma hypothesis,which assumes that(i)the radiation is mainly generated by Langmuir waves via nonlinear processes and(ii)the radiation has frequencies close to the local plasma frequency and/or its second harmonic in the source region. We feel strongly that it is time to advocate an alternative approach without recourse to the plasma hypothesis.This brief discussion explains why.     

A comparative study on 3-D solar wind structure observed by Ulysses and MHD simulation

Ulysses, which was a joint NASA/ESA probe to studythe sun and launched in October of 1990, has been thefirst spacecraft to explore the high latitudinal regions ofheliosphere till now[1]. One of its main scientific purposeswas to observe the latitudinal structures of solar wind pa-rameters, such as velocity, density, mass flux, magneticfield, etc.[1―4]. During its first rapid pole-to-pole transitcovering heliographic latitudes of ±80° from September of1994 to June of 1995, Ulysses observ…     

Gravitationally redshifted absorption lines in the X-ray burst spectra of a neutron star

The fundamental properties of neutron stars provide a direct test of the equation of state of cold nuclear matter, a relationship between pressure and density that is determined by the physics of the strong interactions between the particles that constitute the star. The most straightforward method of determining these properties is by measuring the gravitational redshift of spectral lines produced in the neutron star photosphere. The equation of state implies a mass-radius relation, while a measurement of the gravitational redshift at the surface of a neutron star provides a direct constraint on the mass-to-radius ratio. Here we report the discovery of significant absorption lines in the spectra of 28 bursts of the low-mass X-ray binary EXO0748-676. We identify the most significant features with the Fe XXVI and XXV n = 2-3 and O VIII n = 1-2 transitions, all with a redshift of z = 0.35, identical within small uncertainties for the respective transitions. For an astrophysically plausible range of masses (M approximately 1.3-2.0 solar masses; refs 2-5), this value is completely consistent with models of neutron stars composed of normal nuclear matter, while it excludes some models in which the neutron stars are made of more exotic matter.     

Structure in the early afterglow light curve of the gamma-ray burst of 29 March 2003

Gamma-ray bursts (GRBs) are energetic explosions that for 0.01-100 s are the brightest gamma-ray sources in the sky. Observations of the early evolution of afterglows are expected to provide clues about the nature of the bursts, but their rapid fading has hampered such studies; some recent rapid localizations of bursts have improved the situation. Here we report an early detection of the very bright afterglow of the burst of 29 March 2003 (GRB030329). Our data show that, even early in the afterglow phase, the light curve shows unexpectedly complicated structures superimposed on the fading background.