毫秒脉冲星的高能辐射

 根据自恰毫秒脉冲星磁层外隙模型讨论毫秒脉冲星的高能辐射机制.其中X射线由2个热成分和1个幂律成分组成,γ射线由外隙粒子同步-曲率辐射产生.在此基础上,理论计算了11颗X射线波段及其他39颗在射电波段观测到的毫秒脉冲星,所得理论与观测符合较好,表明该模型能较好地解释毫秒脉冲星的高能辐射机制.     

年轻脉冲星的X-射线非热辐射

年轻的转动驱动脉冲星有较高的自转能损率(Lsd≥1036erg.s-1),而且都有非常高的非热X-射线辐射,利用新的外间隙模型,计算年轻脉冲星的非热X-射线光度,并与观测到的17颗年轻脉冲星的非热X-射线光度能量范围为2~10 keV的观测结果进行比较,模型的计算结果和观测数据吻合较好.     

老年X-射线脉冲星的辐射特性

利用新的外间隙模型,研究计算了老年脉冲星的非热X-射线光度,并与Chandra观测到的七颗老年脉冲星的非热X-射线光度的观测结果进行了比较,模型的计算结果和观测数据吻合较好,同时计算了老年脉冲星可能的伽玛射线光度和流量。     

半群DOPD(n,r)的秩和相关秩

设自然数n≥3,DOPD_n是有限链[n]上的保序且保距部分一一奇异降序变换半群.对任意的r（0≤r≤n-1）,记DOPD（n,r）={α∈DOPD_n：|Im（α）|≤r}为半群DOPD_n的双边星理想.通过对秩为r的元素和星格林关系的分析,获得了半群DOPD（n,r）的极小生成集和秩.确定了当0≤l≤r时,半群DOPD（n,r）关于其星理想DOPD（n,l）的相关秩.     

电磁作用常数α值及电子“反常荷”计算

 用Dirac大数D,Planck大数A唯象地计算了电磁相互作用常数α值,结果与惯用值很好相符.在轻子的亚夸克结构动态模型中,因亚夸克运动使轻子发生等体积表面形变产生电磁作用对称破缺,从而产生“反常质量”,“反常电荷”,则α值将不再是常数,是可变的.由Δm_e反>可计算ΔQ_e反反的值,由Δm_e反>和ΔQ_e反反算出的“反常磁矩”,与实验值相近.最后也讨论了Planck尺度的量子条件.     

颗粒滚动阻力本构参数标定试验研究

针对颗粒滚动阻力本构参数难以通过阻力测量试验来直接标定，开展了两种离散元滚动阻力模型MDEM（modified discrete element method）和HDEM（hysteresis discrete element method）参数的试验标定方法研究。利用自由滚动颗粒的摆动过程建立了颗粒间滚动刚度系数K_r与滚动阻尼系数C_r的试验标定公式，搭建了激光位移传感器测量颗粒微振动的光学试验平台，通过测量试件摆动时程曲线实现了MDEM模型中K_r和C_r的标定；提出基于材料单轴循环拉伸试验的标定方法，利用颗粒本体材料加卸载循环作用下的滞回曲线实现了HDEM模型中的弹性滞后系数 β的标定。试验结果表明，该试验方法能够有效地标定颗粒间滚动阻力本构参数。     

新的f(R)黑洞

f（R）引力是一个直接拓展广义相对论的修正引力理论,它的拉格朗日量是一个仅含曲率标量R的任意函数f（R）.在F（r）=1+αr的条件下（F（r）≡（df（R（r）））/（dr）和αr是一个对广义相对论小的修正量）,导出了度规f（R）引力理论中场方程的精确球对称真空解.此外,考虑了这个黑洞背景时空中的标量场扰动.用六阶WKB （Wentzel-Kramers-Brillouin）方法,讨论了拟正则模和这个黑洞的参数之间的关系,得出这个黑洞是稳定的结论.     

半群OI(n,r)k的秩和相关秩

设自然数n≥3,OI_n^k是有限链[n]上的双边k型-保序严格部分一一变换半群.对任意的1≤k≤n-1,0≤r≤n-1,记OI_（n,r）^k={α∈OI_n^k：|im（α）|≤r}为半群OI_n^k的双边理想.通过对秩为r的元素和格林关系的分析,分别获得了半群OOI_（n,r）^k的极小生成集和秩.进一步确定了当0≤l≤r时,半群OI_（n,r）^k关于其理想OI_（n,l）^k的相关秩.     

一种基于泊松分布的提高X射线脉冲星脉冲轮廓信噪比的方法

论述了X射线脉冲星辐射模型和脉冲轮廓构造算法,提出了以Kullback-leibler距离函数作为评价标准,提高具有泊松分布规律的X射线脉冲星脉冲轮廓信噪比的平滑算法,推导了平滑参数和平滑累积脉冲轮廓的计算公式.搭建了X射线脉冲星导航地面模拟系统,实现了对模拟X射线脉冲星单光子到达时间的记录及X射线脉冲星脉冲轮廓的构造,得到了X射线脉冲到达时间TOA.在X射线脉冲星导航地面模拟系统上,对平滑算法进行了验证,结果表明该算法对于提高累积脉冲轮廓的信噪比效果显著,信噪比提高大于10dB.     

含氮杂环类润滑油添加剂抗磨损性能的神经网络研究

为研究含氮杂环衍生物对三羟甲基丙烷油酸酯改性后的抗磨损性能,计算30个含氮杂环衍生物的分子结构指数. 优化筛选其中分子连接性指数⁴X和⁵X、分子形状指数K₃、电性拓扑状态指数E₇、电性距离矢量M₆和M₁₈. 对以上6种结构指数与磨损量度进行回归分析,将分子结构指数作为神经网络的输入变量,磨损量度作为输出变量,采用6∶2∶1的网络结构,建构预测磨损量度能力较强的神经网络预测模型,模型的总相关系数r_t为0.9921. 计算得到磨损量度的预测值与实验值吻合度较好,相对平均误差为0.38%. 从构建的模型可以看出,—CH₃、=CH—、—NH—等基团的数量及连接方式是影响润滑油磨损量度大小的主要因素.     

Optical pulsations from the anomalous X-ray pulsar 4U0142+61

Anomalous X-ray pulsars (AXPs) differ from ordinary radio pulsars in that their X-ray luminosity is orders of magnitude greater than their rate of rotational energy loss, and so they require an additional energy source. One possibility is that AXPs are highly magnetized neuron stars or 'magnetars' having surface magnetic fields greater than 10(14) G. This would make them similar to the soft gamma-ray repeaters (SGRs), but alternative models that do not require extreme magnetic fields also exist. An optical counterpart to the AXP 4U0142+61 was recently discovered, consistent with emission from a magnetar, but also from a magnetized hot white dwarf, or an accreting isolated neutron star. Here we report the detection of optical pulsations from 4U0142+61. The pulsed fraction of optical light (27 per cent) is five to ten times greater than that of soft X-rays, from which we conclude that 4U0142+61 is a magnetar. Although this establishes a direct relationship between AXPs and the soft gamma-ray repeaters, the evolutionary connection between AXPs, SGRs and radio pulsars remains controversial.     

An optical counterpart to the anomalous X-ray pulsar 4U0142+61

The energy source of the anomalous X-ray pulsars (AXPs) is not understood, hence their designation as anomalous. Unlike binary X-ray pulsars, no companions are seen, so the energy cannot be supplied by accretion of matter from a companion star. The loss of rotational energy, which powers radio pulsars, is insufficient to power AXPs. Two models are generally considered: accretion from a large disk left over from the birth process, or decay of a very strong magnetic field (10(15) G) associated with a 'magnetar'. The lack of counterparts at other wavelengths has hampered progress in our understanding of these objects. Here we report deep optical observations of the field around 4U0142+61, which is the brightest AXP in X-rays. The source has no associated supernova remnant, which, together with its spin-down timescale of approximately 10(5) yr (ref. 5), suggests that it may be relatively old. We find an object with peculiar optical colours at the position of the X-ray source, and argue that it is the optical counterpart. The optical emission is too faint to admit the presence of a large accretion disk, but may be consistent with magnetospheric emission from a magnetar.     

Magnetar-like X-ray bursts from an anomalous X-ray pulsar

Anomalous X-ray pulsars (AXPs) are a class of rare X-ray emitting pulsars whose energy source has been perplexing for some 20 years. Unlike other X-ray emitting pulsars, AXPs cannot be powered by rotational energy or by accretion of matter from a binary companion star, hence the designation 'anomalous'. Many of the rotational and radiative properties of the AXPs are strikingly similar to those of another class of exotic objects, the soft-gamma-ray repeaters (SGRs). But the defining property of the SGRs--their low-energy-gamma-ray and X-ray bursts--has not hitherto been observed for AXPs. Soft-gamma-ray repeaters are thought to be 'magnetars', which are young neutron stars whose emission is powered by the decay of an ultra-high magnetic field; the suggestion that AXPs might also be magnetars has been controversial. Here we report two X-ray bursts, with properties similar to those of SGRs, from the direction of the anomalous X-ray pulsar 1E1048.1 - 5937. These events imply a close relationship (perhaps evolutionary) between AXPs and SGRs, with both being magnetars.     

中国冬季降水对东亚春季O3强弱信号的响应

 利用欧洲中心(ECMWF)ERA-Interim提供的1979—2013年的O₃、温度和位势高度逐月资料及国家气候中心的160站的逐月降水资料,采用EOF分析、相关分析和合成差值分析等方法,分析了东亚春季臭氧的时空变化特征及中国冬季降水对东亚春季O3强弱信号的响应.研究发现：①通过EOF分析可知,东亚春季O₃主要有3种变化特征：其一是东亚春季不同时间的O₃随着纬度的增加而增加（或减少）.其二是青藏高原是一个O₃异常信号较强的地区.其三是鄂霍次克海以西的内陆地区和中国东北部地区的春季O₃异常信号最强,且这两地区的异常信号位相相反.②东亚春季O₃强时,中国冬季降水从西到东呈现了“多-少-多-少-多-少”的分布.这种响应显著的区域位于北方和内陆地区,而中国的东南地区较弱.这就说明,东亚春季O₃对中国冬季降水是有一定的影响的.O₃是如何引起中国冬季降水出现这种波列分布的原因尚有待于进一步的研究.③选取了6个层次分别代表平流层和对流层来开展研究.从相应于O₃强弱年的温压场分析来看,北半球冬季的温度场和位势高度场的合成差值在中高纬度都呈现了波列的分布,在平流层呈“正-负-正”分布,在对流层呈“负-正-负-正-负”分布,且这种温压场对O₃变化的响应在50、100、500hPa和700hPa层次最为显著.据此推测,东亚春季O3变化会引起北半球的温度场和位势高度场的调整,从而使得中国冬季降水分布出现异常.
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稀土元素Gd、Ho和Dy在磁共振成像应用的研究进展

Gd、Ho和Dy因其独特的光学和磁学性质而在生物成像等方面有着广泛的应用.在镧系元素中,Gd~(3+)具有7个不成对的电子,可以提供高的弛豫度,已被广泛地用于磁共振成像(MRI)造影剂,而Ho~(3+)和Dy~(3+)具有最短的电子弛豫时间和最高的有效磁矩,因此有良好的高场T_2弛豫效果.介绍了基于这3种稀土元素的纳米材料在MRI方面的应用.     

分数阶微分方程边值问题正解的存在性

利用不动点指数理论,在相应线性算子的第一特征值的条件下,对下面的分数阶微分方程建立了正解的存在性定理Dα0+u(t)+f(t,u(t))=0,0相似文献   

分数阶微分包含反周期边值问题解的存在性

利用不动点定理,研究了带有反周期边值分数阶微分包含问题{cDαy(t)∈F(t,y(t)),t∈[0,T],T0,2α≤3,y(0)=-y(T),cDpy(0)=-cDpy(T),cDqy(0)=-cDqy(T),解的存在性,所得结果将已有的单值结果推广到多值情形.     

异步轧制无取向硅钢的再结晶织构演变

在无取向硅钢冷轧过程中采用同步轧制和速比为1.06,1.125,1.19的异步轧制,以考察异步轧制对冷轧和再结晶织构的影响.研究发现,异步轧制减弱冷轧织构中{001}～{112}〈110〉组分,增强{111}〈112〉并减弱{111}〈110〉组分.{111}〈112〉和{111}～{225}〈110〉形变晶粒内剪切带处分别形成η(〈001〉∥RD)及偏离其15°的η′(Ψ=75°,θ=0～45°,φ=0°)再结晶晶粒,η′因晶核尺寸优势发展成为主要织构组分.异步轧制下形变织构的变化有利于改善再结晶织构特征及性能,其影响随速比增大而增强.     

Transient pulsed radio emission from a magnetar

Anomalous X-ray pulsars (AXPs) are slowly rotating neutron stars with very bright and highly variable X-ray emission that are believed to be powered by ultra-strong magnetic fields of >10(14) G, according to the 'magnetar' model. The radio pulsations that have been observed from more than 1,700 neutron stars with weaker magnetic fields have never been detected from any of the dozen known magnetars. The X-ray pulsar XTE J1810-197 was revealed (in 2003) as the first AXP with transient emission when its luminosity increased 100-fold from the quiescent level; a coincident radio source of unknown origin was detected one year later. Here we show that XTE J1810-197 emits bright, narrow, highly linearly polarized radio pulses, observed at every rotation, thereby establishing that magnetars can be radio pulsars. There is no evidence of radio emission before the 2003 X-ray outburst (unlike ordinary pulsars, which emit radio pulses all the time), and the flux varies from day to day. The flux at all radio frequencies is approximately equal--and at >20 GHz XTE J1810-197 is currently the brightest neutron star known. These observations link magnetars to ordinary radio pulsars, rule out alternative accretion models for AXPs, and provide a new window into the coronae of magnetars.     

缝隙连接阻断剂18α-甘草次酸对大鼠血管平滑肌细胞增殖的作用

为探讨缝隙连接是否参与抑制大鼠血管平滑肌细胞的增殖及可能的分子机制,本研究以原代及传代培养大鼠胸主动脉平滑肌细胞为模型,实验分2组：对照组、缝隙连接阻断剂18α-甘草次酸（18α-—Glycyrrhetinicacid,18Q—GA）组。MTT法及流式细胞术检测细胞的增殖活性,染料示踪分子传递法（划痕标记染料传输法）检测细胞的缝隙连接功能,Westernblotting法检测细胞中缝隙连接蛋白40（Cx40）和43（Cx43）表达。结果显示：（1）与对照组相比,18α-GA组MTT法测得的氏,。值及细胞周期S期比例均降低（P〈0．01）,细胞增殖活性减弱;（2）与对照组相比,18α-GA组罗氏黄荧光染料传递百分数显著降低,缝隙连接功能明显减弱（P〈0．01）;（3）与对照组相比,18rGA组Cx40和总Cx43蛋白表达无显著差异（P〉0．05）,磷酸化Cx43与非磷酸化Cx43的比值显著降低（P〈0．01）。由此可知,18α-GA可能主要通过下调血管平滑肌细胞磷酸化Cx43蛋白表达,引起缝隙连接通讯功能减弱,从而抑制了血管平滑肌细胞的增殖。