TS—1沸石合成过程中模板剂用量对钛进入骨架的影响

以ＴＰＡＢｒ为模板剂、ＮＨ３．Ｈ２Ｏ为碱源，水热条件下合成了ＴＳ－１沸石，采用ＸＲＤ、ＩＲ、ＵＶ－Ｖｉｓ、＾２９ＳｉＣＰＭＡＳＮＭＲ、＾２７ＡｌＣＭＡＳＮＭＲ、＾１３ＣＣＰＭＡＳＮＭＲ等表征手段详细研究了模板剂不同用量对钛进入骨架的影响。     

COHERENT OSCILLATORY WAVES FOR MULTIDIMENSIONAL HYPERBOLIC SYSTEMS

ＣＯＨＥＲＥＮＴＯＳＣＩＬＬＡＴＯＲＹＷＡＶＥＳＦＯＲＭＵＬＴＩＤＩＭＥＮＳＩＯＮＡＬＨＹＰＥＲＢＯＬＩＣＳＹＳＴＥＭＳＣｈｅｎＭｉｎｇ１）ＱｉｕＱｉｎｇｊｉｕ２）（１）ＤｅｐａｒｔｍｅｎｔｏｆＲａｄｉｏＥｎｇｉｎｅｅｒｉｎｇ，ＳｏｕｔｈｅａｓｔＵ...     

最新MOTOROLA V998+手机电源电路介绍及开机过程

ＭＯＴＯＲＯＬＡＶ９９８+手机的电源及音频处理模块由一块ＧＣＡＰ（Ｕ９００）完成,ＥＰＲＯＭＴ和ＥＥＰＲＯＭ由一块Ｕ７０１完成,ＳＹＮ-ＭＤＥＭ（频率合成及调制节调）由一块ＭＡＧＩＣ（Ｕ９１３）完成。逻辑控制ＣＰＵ是ＷＨＩＴＥＣＡＰ（Ｕ７００）。１介绍各个电压在逻辑控制下的先后产生过程１．１Ｂ+电压当ＥＸＴ-Ｂ+供电时,Ｕ９００的Ｆ１０脚输出高电平,Ｑ９４２的Ｓ-Ｄ截止,Ｂ+由ＥＸＴ—Ｂ+产生。当ＢＡＴＴ+供电时,Ｆ１０脚输出低电平,Ｑ９４２的Ｓ-Ｄ导通,Ｂ+由ＢＡＴＴ+产生。ＣＲ９４０为隔离二极管。１．２Ｖ-Ｂ０…     

用PCR扩增和克隆鸡贫血病毒衣壳蛋白VP2基因

接种鸡贫血病毒（ＣＡＶ）Ｃｕｘ－１毒株于ＭＤＣＣ－ＲＰ１细胞中,并用经狄高辛标记的ＣＡＶ衣壳蛋白ＶＰ１基因克隆ＤＮＡ作为探针在斑点杂交中检测和比较了各代细胞中ＣＡＶ ＤＮＡ水平。通过聚合酶链式反应（ＰＣＲ）,从ＣＡＶ ＤＮＡ水平较高的ＭＤＣＣ－ＲＰ１细胞基因组ＤＮＡ中扩增出ＣＡＶ衣壳蛋白ＶＰ２基因片段约６５０ｂｐ的编码序列,将该ＰＣＲ扩增的产物于ＥｃｏＲＩ和ＫｐｎＩ位点克隆到ｐＵＣ１９质粒载体中,     

单－6－（咪唑－1－基）－β－环糊精的合成

由β－ＣＤ—ＯＴｓ或β－ＣＤ－Ｉ在ＤＭＦ中，和过量咪唑反应，合成了单－６－（咪唑－１－基）－β－环糊精（简称β－ＤＣ－Ｉｍ）．产率较高，分别为６０％和６２％．并对化合物的结构进行了ＴＬＣ、ＩＲ、ＵＶ、１ＨＮＭＲ及元素分析等确证．其中ＵＶ数据未见文献报道．     

QWF－1型汽车尾气分析仪配装自动记录仪的研制

ＱＷＦ－１型汽车尾气分析仪配装自动记录仪的研制ＤＥＶＥＬＯＰＭＥＮＴＯＮＴＨＥＡＴＴＡＣＨＥＤＡＵＴＯＭＡＴＩＣＲＥＣＯＲＤＤＩＡＬＯＦＭＯＤＥＬＱＷＦ－１ＡＵＴＯＴＡＩＬ－ＧＡＳＡＮＡＬＹＳＩＳＡＰＰＡＲＡＴＵＳＬｉＬｉａｎｇｅｒＣｈｅｎＪｉａｎｂ...     

ESTABLISHING AN ORGANIC CHEMISTRY MICROSCALE LABORATORY PROGRAM

ＥＳＴＡＢＬＩＳＨＩＮＧＡＮＯＲＧＡＮＩＣＣＨＥＭＩＳＴＲＹＭＩＣＲＯＳＣＡＬＥＬＡＢＯＲＡＴＯＲＹＰＲＯＧＲＡＭ￥ＡｒｔｈｕｒＲ．Ｍｕｒｄｏｃｈ（ＭｏｕｎｔＵｎｉｏｎＣｏｌｌｅｇｅ，Ａｌｌｉａｎｃｅ，Ｏｈｉｏ，ＵＳＡ）（Ｖｉｓｉｔｉｎｇｐｒｏｆｅｓ...     

碳核价夸克与海夸克分布的核效应

提出了一个由１－Ａ的深度非弹性散射和核Ｄｒｅｌ－Ｙａｎ过程的实验数据得到价夸克分布和海夸克分布的核效应的函数ＲＡＶ（ｘｔ）和ＲＡｓ（ｘｔ）的方法。这两个函数可以用来检验核子结构的核效应的理论模型。文中以碳核为例求出了ＲＣｖ（ｘｔ）和ＲＣｓ（ｘｔ）。     

关于高校内部管理的四个标准

关于高校内部管理的四个标准ＯＮＦＯＵＲＣＲＩＴＥＲＩＡＯＦＴＨＥＩＮＴＥＲＩＯＲＭＡＮＡＧＥＭＥＮＴＯＦＴＨＥＵＮＩＶＥＲＳＩＴＩＥＳＡＮＤＣＯＬＬＥＧＥＳＣｈｅｎＺｈａｎｇｍｉｎｇ（ＺｈｅｊｉａｎｇＦｉｓｈｅｒｉｅｓＣｏｌｌｅｇｅ，Ｚｈｏｕｓｈａｎ...     

二苯骈四氮杂[14]轮烯金属配合物合成及酰化反应的研究

本文合成了５，１４－二氢－６，８，１５，１７－四甲基二苯骈〔ｂ．ｉ〕〔１，４，８，１１〕四氮杂〔１４〕轮烯金属配合物ＴＭＴＡＡＮｉ（Ⅱ），ＴＭＴＡＡＣｕ（Ⅱ）和ＴＭＴＡＡＶ＝０。这类分子结构中，金属离子Ｍ（Ⅱ）的对位碳原子上可发生亲电取代反应，如酰化反应，获得了十个酰化产物，并通过元素分析，＾１ＨＮＭＲ，ＥＰＲ等方法进行了表征，酰化反应的发生说明了这类金属配合物的类芳香性，并为改善这类大环金属配合     

Nuclear-powered millisecond pulsars and the maximum spin frequency of neutron stars

Millisecond pulsars are neutron stars that are thought to have been spun-up by mass accretion from a stellar companion. It is not known whether there is a natural brake for this process, or if it continues until the centrifugal breakup limit is reached at submillisecond periods. Many neutron stars that are accreting mass from a companion star exhibit thermonuclear X-ray bursts that last tens of seconds, caused by unstable nuclear burning on their surfaces. Millisecond-period brightness oscillations during bursts from ten neutron stars (as distinct from other rapid X-ray variability that is also observed) are thought to measure the stellar spin, but direct proof of a rotational origin has been lacking. Here we report the detection of burst oscillations at the known spin frequency of an accreting millisecond pulsar, and we show that these oscillations always have the same rotational phase. This firmly establishes burst oscillations as nuclear-powered pulsations tracing the spin of accreting neutron stars, corroborating earlier evidence. The distribution of spin frequencies of the 11 nuclear-powered pulsars cuts off well below the breakup frequency for most neutron-star models, supporting theoretical predictions that gravitational radiation losses can limit accretion torques in spinning up millisecond pulsars.     

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.     

引力子质量对中子星I-Q关系的修正

近年来,研究发现中子星的转动惯量I和四极矩Q存在着一个关系式,即I-Q关系.而且,该关系式不依赖于中子星内部的物态方程,与引力理论相关.因此,对该关系式的研究可用来检验引力理论.de Rham-GabadadzeTolley(dRGT)massive gravity是一种自洽的引力子静止质量不为零的修正引力理论,是目前国际引力理论研究的热点.本论文主要基于该修正引力理论,在慢速旋转近似下,利用多方指数n=0的物态方程,计算了dRGT massive gravity中牛顿极限下的I-Q关系.我们将dRGT massive gravity与爱因斯坦引力中的I-Q关系进行比较,发现引力子质量不会影响I与Q的平方之间无量纲化后的正比关系,但会改变其比例系数.     

超子对中子星的影响

通过相对论平均场模型以及弱相互作用理论研究∑超子对中子星的影响。结果表明,∑超子对三种介子场均有影响,进而改变了中子星内部的粒子分布、质量——半径关系等。∑超子在冷却方面的效应更加明显,一方面,它们改变电子和肚子的直接Urca过程的发生范围,另一方面也使得中微子发射率大幅降低,因此∑超子可能并不利于中子星冷却。     

原初典型恒星及其星核黑洞的形成、演化和结构的基本规律

本文在文献[1]、[2]的基础上,应用相对论性牛顿万有引力定律,对原初典型恒星及其星核M。黑洞的形成、演化和结构,作了更深入的探索研究．得到了一系列很有意义的结果：1、导出了原初典型恒星Mo及其星核Ms黑洞质量的上界和下界．进而导出了原初典型恒星在其简并中子黑涧（Mos=Mo）态下一分为二的死亡大爆炸中释放能量的上下界（即超新星爆发所释放能量的上下界）;2、导出了星核Ms黑洞独有的一系列鼎级极限物理特性．导出了黑洞无内阻理想流体的超流效应及黑洞吸集粒子的经纬分流的筛选效应．证明了星核Ms黑洞是具有不再爆炸、不再坍缩、不再发射的“三不”特性的稳定天体;3、在相对论性引力理论框架内,证明了光速最大原理;4、导出了原初典型恒星在一分为二的死亡大爆炸中静质量Mo、场（暗）质量△MG的结构和分布规律．揭示了星核Ms黑洞结构的奥秘;5、导出了恒星、星系、总星系等典型层次天体的真空中场（暗）质量的分布规律．     

The formation of stars by gravitational collapse rather than competitive accretion

There are two dominant models of how stars form. Under gravitational collapse, star-forming molecular clumps, of typically hundreds to thousands of solar masses (M(o)), fragment into gaseous cores that subsequently collapse to make individual stars or small multiple systems. In contrast, competitive accretion theory suggests that at birth all stars are much smaller than the typical stellar mass (approximately 0.5M(o)), and that final stellar masses are determined by the subsequent accretion of unbound gas from the clump. Competitive accretion models interpret brown dwarfs and free-floating planets as protostars ejected from star-forming clumps before they have accreted much mass; key predictions of this model are that such objects should lack disks, have high velocity dispersions, form more frequently in denser clumps, and that the mean stellar mass should vary within the Galaxy. Here we derive the rate of competitive accretion as a function of the star-forming environment, based partly on simulation, and determine in what types of environments competitive accretion can occur. We show that no observed star-forming region can undergo significant competitive accretion, and that the simulations that show competitive accretion do so because the assumed properties differ from those determined by observation. Our result shows that stars form by gravitational collapse, and explains why observations have failed to confirm predictions of the competitive accretion model.     

A circumstellar disk associated with a massive protostellar object

The formation process for stars with masses several times that of the Sun is still unclear. The two main theories are mergers of several low-mass young stellar objects, which requires a high stellar density, or mass accretion from circumstellar disks in the same way as low-mass stars are formed, accompanied by outflows during the process of gravitational infall. Although a number of disks have been discovered around low- and intermediate-mass young stellar objects, the presence of disks around massive young stellar objects is still uncertain and the mass of the disk system detected around one such object, M17, is disputed. Here we report near-infrared imaging polarimetry that reveals an outflow/disk system around the Becklin-Neugebauer protostellar object, which has a mass of at least seven solar masses (M(o)). This strongly supports the theory that stars with masses of at least 7M(o) form in the same way as lower mass stars.     

A neutron-star-driven X-ray flash associated with supernova SN 2006aj

Supernovae connected with long-duration gamma-ray bursts (GRBs) are hyper-energetic explosions resulting from the collapse of very massive stars ( approximately 40 M\circ, where M\circ is the mass of the Sun) stripped of their outer hydrogen and helium envelopes. A very massive progenitor, collapsing to a black hole, was thought to be a requirement for the launch of a GRB. Here we report the results of modelling the spectra and light curve of SN 2006aj (ref. 9), which demonstrate that the supernova had a much smaller explosion energy and ejected much less mass than the other GRB-supernovae, suggesting that it was produced by a star whose initial mass was only approximately 20 M\circ. A star of this mass is expected to form a neutron star rather than a black hole when its core collapses. The smaller explosion energy of SN 2006aj is matched by the weakness and softness of GRB 060218 (an X-ray flash), and the weakness of the radio flux of the supernova. Our results indicate that the supernova-GRB connection extends to a much broader range of stellar masses than previously thought, possibly involving different physical mechanisms: a 'collapsar' (ref. 8) for the more massive stars collapsing to a black hole, and magnetic activity of the nascent neutron star for the less massive stars.     

Unbound or distant planetary mass population detected by gravitational microlensing

Since 1995, more than 500 exoplanets have been detected using different techniques, of which 12 were detected with gravitational microlensing. Most of these are gravitationally bound to their host stars. There is some evidence of free-floating planetary-mass objects in young star-forming regions, but these objects are limited to massive objects of 3 to 15 Jupiter masses with large uncertainties in photometric mass estimates and their abundance. Here, we report the discovery of a population of unbound or distant Jupiter-mass objects, which are almost twice (1.8(+1.7)(-0.8)) as common as main-sequence stars, based on two years of gravitational microlensing survey observations towards the Galactic Bulge. These planetary-mass objects have no host stars that can be detected within about ten astronomical units by gravitational microlensing. However, a comparison with constraints from direct imaging suggests that most of these planetary-mass objects are not bound to any host star. An abrupt change in the mass function at about one Jupiter mass favours the idea that their formation process is different from that of stars and brown dwarfs. They may have formed in proto-planetary disks and subsequently scattered into unbound or very distant orbits.     

Soft equations of state for neutron-star matter ruled out by EXO 0748 - 676

The interiors of neutron stars contain matter at very high densities, in a state that differs greatly from those found in the early Universe or achieved in terrestrial experiments. Matter in these conditions can only be probed through astrophysical observations that measure the mass and radius of neutron stars with sufficient precision. Here I report a determination of the mass and radius of the neutron star EXO 0748 - 676 that appears to rule out all the soft equations of state of neutron-star matter. If this object is typical, then condensates and unconfined quarks do not exist in the centres of neutron stars.