Tugboat model for OB binaries, X-ray stars and pulsars

An examination of the kinematical properties of binary OB stars, binary X-ray sources and pulsars suggests an evolutionary sequence linking an apparent low-velocity class of pulsars to the binary nature of their extreme Population I progenitors.     

Profile of the composition fractions in neutron stars

The composition fractions of β-stable neutron stars and their radial distributions are investigated based on Skyrme-Hartree-Fock theory and Tolman-Oppenheimer-Volkoff (TOV) equation. It is found that a pure neutron interior with a radius of 3.5 km can exist in the neutron stars. When the radius is greater than 3.5 km, the fractions of the proton, electron and μ⁻ appear and increase with the increment of the radius, then decrease after reaching their maximum at the radius of 8 km. These results make it possible to further study the thermal evolution and magnetic properties of the neutron stars.     

大质量中子星的冷却性质探讨

鉴于近期的观测数据更倾向于大质量的中子星,通过相对论平均场理论和相关弱作用理论来研究大质量中子星内部中微子发射性质及星体的冷却曲线.计算结果表明大质量中子星的冷却性质与星体质量有关,但是具体的变化规律还取决于模型参数.     

An efficient photoelectric X-ray polarimeter for the study of black holes and neutron stars

The study of astronomical objects using electromagnetic radiation involves four basic observational approaches: imaging, spectroscopy, photometry (accurate counting of the photons received) and polarimetry (measurement of the polarizations of the observed photons). In contrast to observations at other wavelengths, a lack of sensitivity has prevented X-ray astronomy from making use of polarimetry. Yet such a technique could provide a direct picture of the state of matter in extreme magnetic and gravitational fields, and has the potential to resolve the internal structures of compact sources that would otherwise remain inaccessible, even to X-ray interferometry. In binary pulsars, for example, we could directly 'see' the rotation of the magnetic field and determine if the emission is in the form of a 'fan' or a 'pencil' beam. Also, observation of the characteristic twisting of the polarization angle in other compact sources would reveal the presence of a black hole. Here we report the development of an instrument that makes X-ray polarimetry possible. The factor of 100 improvement in sensitivity that we have achieved will allow direct exploration of the most dramatic objects of the X-ray sky.     

超子同位旋相互作用对中子星转动惯量的影响

 利用相对论平均场理论,考虑重子八重态{n,p,Λ, Σ^-, Σ⁰, Σ⁺,Ξ^-,Ξ⁰},研究了超子同位旋相互作用对中子星转动惯量的影响.研究发现:考虑到超子同位旋相互作用,当x_ρ 分别取2,1,2/3时,中子星的转动惯量依次减小,同一中子星质量以及当半径R>13.961km时同一中子星半径所对应的转动惯量也均依次减小;而当半径R<13.961km时,对同一中子星半径所对应的转动惯量来说,x_ρΣ=2/3对应的转动惯量最小,x_ρΣ=2所对应的较大,而x_ρΣ=1 相应的转动惯量最大.     

强磁场下中子星外壳层的电子俘获

 以核素⁵⁶Co和⁵⁹Fe为例,讨论了强磁场中子星外壳层电子俘获.结果表明,绝大部分中子星表面的磁场范围10⁴~10⁹T,磁场对电子俘获率的影响很小.对于一些磁场范围为10⁹~10¹⁴T的超磁星,磁场可使电子俘获率大大降低,甚至可以降低3个量级.     

Detectable radio flares following gravitational waves from mergers of binary neutron stars

Mergers of neutron-star/neutron-star binaries are strong sources of gravitational waves. They can also launch subrelativistic and mildly relativistic outflows and are often assumed to be the sources of short γ-ray bursts. An electromagnetic signature that persisted for weeks to months after the event would strengthen any future claim of a detection of gravitational waves. Here we present results of calculations showing that the interaction of mildly relativistic outflows with the surrounding medium produces radio flares with peak emission at 1.4 gigahertz that persist at detectable (submillijansky) levels for weeks, out to a redshift of 0.1. Slower subrelativistic outflows produce flares detectable for years at 150 megahertz, as well as at 1.4 gigahertz, from slightly shorter distances. The radio transient RT 19870422 (ref. 11) has the properties predicted by our model, and its most probable origin is the merger of a compact neutron-star/neutron-star binary. The lack of radio detections usually associated with short γ-ray bursts does not constrain the radio transients that we discuss here (from mildly relativistic and subrelativistic outflows) because short γ-ray burst redshifts are typically >0.1 and the appropriate timescales (longer than weeks) have not been sampled.     

中子星壳层中强磁场与β衰变

 基于原子核壳层模型,分析了在强磁场作用下中子星壳层中的β衰变率,并以反应⁶³Co(β^-)⁶³Ni为例作详细计算.结果表明:弱磁场对中子星壳层中的β衰变几乎没有影响,强磁场(B>10⁸T)使β衰变率显著增大;同时在相同的磁场强度下,基态的β衰变比激发态的β衰变所受影响更大.这些结论对进一步研究中子星晚期演化和双中子星系统快中子俘获过程的核合成是有意义的.     

多变量频域极大似然辨识算法研究

提出了多变量频域极大似然辨识算法.在单变量频域极大似然辨识算法的基础之上,得出多变量系统的频域极大似然辨识算法,并且优化设计多正弦辨识输入信号.针对大型挠性结构的模型进行了仿真,验证了算法的有效性,同时仿真结果表明:对于挠性结构,多变量频域极大似然辨识算法是有效的,而且能够在较大的频宽、较低信噪比的情况下得到良好的辨识结果.     

挠性结构模型的频域极大似然法辨识

在构建的以压电陶瓷为执行器、电阻式应变片为传感器的挠性悬臂梁物理实验系统基础上,优化设计多正弦辨识输入信号,利用频域极大似然法辨识得到了整个系统的数学模型,并根据该模型进行了数字和物理控制仿真,验证了模型的有效性.良好的控制效果表明:对于挠性结构,频域极大似然法是一种有效的模型辨识方法.     

An increased estimate of the merger rate of double neutron stars from observations of a highly relativistic system

The merger of close binary systems containing two neutron stars should produce a burst of gravitational waves, as predicted by the theory of general relativity. A reliable estimate of the double-neutron-star merger rate in the Galaxy is crucial in order to predict whether current gravity wave detectors will be successful in detecting such bursts. Present estimates of this rate are rather low, because we know of only a few double-neutron-star binaries with merger times less than the age of the Universe. Here we report the discovery of a 22-ms pulsar, PSR J0737-3039, which is a member of a highly relativistic double-neutron-star binary with an orbital period of 2.4 hours. This system will merge in about 85 Myr, a time much shorter than for any other known neutron-star binary. Together with the relatively low radio luminosity of PSR J0737-3039, this timescale implies an order-of-magnitude increase in the predicted merger rate for double-neutron-star systems in our Galaxy (and in the rest of the Universe).     

求解最大特征值及其对应特征向量的FPGA实现

针对某些领域只需求解矩阵的最大特征值及其对应特征向量的特点,设计了基于乘幂法的复矩阵的最大特征值及其对应特征向量求解的FPGA实现,提高了运算速度。设计采用状态机设计方法,将9×9复矩阵的定点数格式转化为浮点数运算,使得到的特征值及特征向量有很高的精度。结果表明,本设计稳定并可实现工程化应用。     

Nucleosynthetic signatures of the first stars

The chemically most primitive stars provide constraints on the nature of the first stellar objects that formed in the Universe; elements other than hydrogen, helium and traces of lithium present within these objects were generated by nucleosynthesis in the very first stars. The relative abundances of elements in the surviving primitive stars reflect the masses of the first stars, because the pathways of nucleosynthesis are quite sensitive to stellar masses. Several models have been suggested to explain the origin of the abundance pattern of the giant star HE0107-5240, which hitherto exhibited the highest deficiency of heavy elements known. Here we report the discovery of HE1327-2326, a subgiant or main-sequence star with an iron abundance about a factor of two lower than that of HE0107-5240. Both stars show extreme overabundances of carbon and nitrogen with respect to iron, suggesting a similar origin of the abundance patterns. The unexpectedly low Li and high Sr abundances of HE1327-2326, however, challenge existing theoretical understanding: no model predicts the high Sr abundance or provides a Li depletion mechanism consistent with data available for the most metal-poor stars.     

基于贝叶斯推断的脉冲星偏振位置角拟合算法

脉冲星辐射束的偏振位置角与相位的关系可用旋转矢量模型(RVM)描述,现有的Levenberg-Marquardt非线性拟合和格点搜寻算法对RVM的拟合存在效率低、易过拟合等问题。本文发展了一套基于贝叶斯推断的马尔可夫链蒙特卡洛算法(MCMC),并用该方法对已有文献中的10颗脉冲星偏振位置角进行了拟合。结果表明,MCMC算法不仅能得到与已有文献一致的结果,而且该算法具有高效、不易过拟合、能更好地估计参数的可信度区间等优点。     

露天矿微差爆破振动对多层建筑的影响

基于十堰市高家沟堰口采石场爆破开挖工程现场试验,对矿山附近一栋多层建筑物进行爆破振动监测,分析了该建筑物不同楼层的振动速度及谐波频率的变化规律。结果表明:爆破远区的多层建筑物受爆破振动影响时,垂直方向振动速度随着楼层高度的增加而变大,水平方向振动速度随着楼层高度的增加而变小;爆破振动产生的谐波频率丰富,较高楼层谐波频率分布范围小于较低楼层且更接近建筑物的固有频率。     

双星和四极振子的引力波

按拉格朗日函数Ｌ＝√－ｇ（λＲ＋αＲμｙＲ＾μｙ＋βＲ＾２－Ｌｍ）的高导数引力理论研究力学系统的引力波问题在α〉０，α＋３β〈０的条件下，求出了双星和线性四极振子激发的引力辐射波，其结果当耦合常数α→０，β→０时，Ｅｉｎｓｔｅｉｎ引力理论的结果相同。     

基于状态分析法的多功能数字毫秒计监控程序设计

以多功能数字毫秒计为例，阐述了如何用状态分析法设计系统监控程序，并给出原理及程序设计的步骤，该方法对于一键多义型系统的监控程序设计，可以使监控程序更加简约化，用这种方法设计的数字毫秒计，真正实现了多功能，更适合大学物理实验教学的需要。