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.     

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.     

The evolution model of the earth’s limited expanding

Based on the prerequisite that the earliest acid rock formed because of the initial global expanding tectonic processes, by combining it with other geological limitation conditions, and starting from the lithosphere elastic mechanics, the following is defined: the earth expansion started at about 4300 Ma ago, the average increasing rate of the earth radius is 0.40 mm/a, the initial expanding earth radius is 4651 km, and the initial global expansion of tectonic processes happened at 4183.7 Ma ago. From the natural and attenuation evolution condition of the earth and terrestrial planets, through the limit condition got from the combination of the mathematics logic and the geological significance, the limited expanding earth evolution model is established as follows: in whichR ₀= 4.651×10⁶ m,A =1.86×10⁶ m, β = -6.01×10⁻¹⁰/ a andt _s=3×10⁸ a. From this model the maximum radiusR _maxof the limited expanding earth evolution should be 6511 km. The earth’s radius increasing rate is about 0.1 mm/a at present.     

流夸克质量对混合星性质的影响

利用强子物质的相对论平均场理论和夸克物质的有效质量口袋模型, 研究流夸克质量的选取对混合星性质的影响. 结果表明, 随着流夸克质量的增大, 强子\|夸克相变使密度变大, 超子种类变多, 混合相区域的状态方程变硬, 中子星的最大质量及半径变大. 当奇异流夸克质量由90 MeV增到200 MeV时, 混合星最大质量由1.4 M⊙增至1.63 M⊙（M⊙=1.99×1030kg为太阳质量）, 半径由10.24 km增至11.64 km.      

π介子凝聚对中子星物质的影响

在相对论平均场理论框架下研究了π^-介子凝聚对包括Δ共振态的中子星物质状态方程及其粒子分布的影响. 研究表明, π^-介子凝聚的存在对中子星物质的粒子分布有明显影响, 使Δ^-粒子出现推迟, Δ⁺粒子出现提前. π^-介子凝聚的出现还使中子星物质的状态方程变软. 尽管这种改变很小, 但这种变软的趋势仍具有重要的意义.     

ρ介子对中子星物态方程的影响

在相对论平均场理论框架内采用σ-ω-ρ模型进行数值计算,确定引入ρ介子对中子星能量密度和压强变化的影响,进而研究其对中子星壳层的物态方程的影响。计算结果表明:ρ介子使中子星能量密度随着重子数密度的增大而增大,同时压强也随着重子数密度的增大而变化更大更显著,从而使中子星的物态方程变硬。     

Δ共振态存在于中子星内部的可能性探讨

本文通过相对论平均场理论和Tolman-Oppenheimer-Volkoff方程来研究中子星的微观和宏观性质。与最新的脉冲星J1614-2230的观测数据作比照,可以发现除了传统的中子星物质外,Δ共振态中的Δ-和Δ0粒子也很可能大量存在于PSR J1614-2230的内部。另外,也进一步探讨了Δ共振态对中子星所产生的影响。     

Isotopic composition characteristics and identification of immature and lowmature oils

Isotopic composition characteristics and the significance of immature and low-mature oils are first systematically discussed. The carbon isotopes of the whole oil can be divided into two groups, one has δ¹³C main peak values ranging from -30‰ to -29 and the other from -27‰ to-25‰, they are related to lacustrine and salt-lake facies or swamp facies, respectively. The carbon isotopic fractionation among different group components is relatively small, usually less than 2‰ and the biggest difference in fractionation often occurs between saturated and aromatic fractions. Their δD values vary between -180‰ and -130‰ The main peak of their δD values concentrates between -170‰ and -150‰, suggesting a domination of lacustrine fades. However, the secondary peak ranges from -160‰ to -150‰, showing a frequent salinization of paleo-water bodies. The average δ¹³C values of the methane vary between -50‰ and -52‰, about 10‰ lighter than those of mature oils. There is a relatively good correlationship between immature and low-mature oils and their source rocks in carbon isotopic compositions of group fractions and monohydrocarbons; moreover, compared with the source rocks of mature oils, that of immature oils is often relatively depleted in¹³C, which is one of the characteristics of immature oils, differing from those of mature oils.     

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.     

Validating global hydrological models by ground and space gravimetry

The long-term continuous gravity observations obtained by the superconducting gravimeters (SG) at seven globally-distributed stations are comprehensively analyzed. After removing the signals related to the Earth’s tides and variations in the Earth’s rotation, the gravity residuals are used to describe the seasonal fluctuations in gravity field. Meanwhile, the gravity changes due to the air pressure loading are theoretically modeled from the measurements of the local air pressure, and those due to land water...     

超子排斥势和弱吸引势对中子星性质的影响

从相对论平均场理论出发,研究了不同超子势下,超子耦合常数对中子星性质的影响．对4种不同的超子势进行了计算,计算发现,∑强排斥势和Ξ的弱吸引势都将抑制超子的产生．作者通过对不同超子势的计算得到以下结果：∑排斥势越强,状态方程越硬,其所得中子星的最大质量越大．计算得到中子星的质量为1．32～1．45M⊙（M⊙为太阳质量）,与实际观测基本符合．     

Suppression intra-channel four-wave mixing by strong dispersion management in 160 Gb/s OTDM RZ 100 km transmission

The effect of intra-channel four-wave mixing on the performance of a 160 Gb/s OTDM RZ 100 km transmission system is analyzed. Strong dispersion management to suppress the detrimental effects of intra-channel four-wave mixing is presented theoretically and verified experimentally. Results demonstrate that amplitude fluctuation and ghost pulses are well suppressed by strong dispersion management. Stable (>2 h) error-free (10-12 ) transmission over 100 km is achieved without forward-error correction, and the power penalty is ～3.6 dB.     

Ultrahigh-pressure (4.5–5.5 GPa) experimental research on pyroxene-garnet transition and its significance

Conclusions The transition from natural Al-enstatite to garnet and Al-poor pyroxene has taken place under the condition of about 1000°C and 4.5–5.5 GPa, and new phases of garnet and corundum have formed when 15% Al₂O₃ was added to the initial natural Al-enstatite. This experimental result has explained the ultrahigh pressure (3.5–5.0 GPa) and relatively low temperature (< 1000°C) genesis of the ultramafic rock of high-pressure metamorphic zone in Dabieshan-northern Jiangsu-Jiaodong and of red corundum garnetite coexisting with garnet peridotite. From the genetic mineralogy, petrology andP-T equilibrium conditions of garnet peridotite of the high-pressure metamorphic zone, kimberlite and Cenozoic basalt and the ultrahigh pressure experimental result, it is inferred that the upper mantle garnet peridotite is transformed with the increase of depth from Al-rich pyroxene garnet peridotite (80–120 km) to Al-poor pyroxene garnet peridotite (greater than 120–150 km).     

"中子星"研究的挑战

脉冲星(PSRs)被发现之后,很快地就被证认为中子星(NSs),关于它们的研究极大地丰富了人们对于自然的认识.由于第一颗射电脉冲星的发现以及对强引力场下广义相对论的检验,脉冲星研究者已经两次获得了诺贝尔物理学奖.最近,"中子星"家族中的一些新种类被发现了,它们是:所谓的软伽马射线重复爆(SGRs),反常X射线脉冲星(AXPs),超新星遗迹(SNRs)中的致密中心天体(CCOs)和暗弱热中子星(DTNs).这对理论家们提出了如下的挑战:是否部分或者全部的所谓"中子星"的本质实际上是"奇异星(SSs)"?是否存在所谓的"磁星"(一种具有超强磁场的中子星)?本文论述了"中子星"的观测特性,为理解它们本质所作的理论努力以及不同模型间的争论(尤其是关于SGRs和AXPs).     

Morphology of polar ionospheric O^＋ ion upflow： FAST observations during quiet time

With energetic ion measurements on FAST satellite, the morphologic features of quiet-time ionospheric O ion upflowing at altitudes of 2000 to 4000 km are drawn out for the first time. The pre-noon cusp/cleft is the predominant region of upflowing occurrence for O with lower energy. Meanwhile the pre-dawn sector near the equatorward edge of the plasma convection dominates the occurrence for the higher energy O ions. No matter whether the energy is lower or higher, the upflows occur often over a wide MLT range of lower latitudes outside the auroral oval. The upflowing within the pre-midnight (21:00― 22:00 MLT) auroral oval carrys larger energy fluxes, with extremely large fluxes for higher energy O appearing near the polar cap boundary. For altitudes of 2000―4200 km under observation, the ion conics occur much more frequently than ion beams. Ion beams are rarely found below 3000 km, while the conics occur uniformly over the observed altitudes.     

Discovery of the superlarge gallium ore deposit in Jungar, Inner Mongolia, North China

Gallium, Ge, V, and U are the associated valuable elements in coal. From the 1950s to the 1970s, some researchers in the departments of coal industry and mineral resources of China investigated these elements in coal during geological explorations. The enrichment mechanism and the environmental influence of trace elements in coal have been deeply studied in recent twenty years. With respect to the ore-forming theories and practical utilizations of metals in coal, germanium was furthest studi…     

Crustal P-wave velocity structure in Lower Yangtze region： Reinterpretation of Fuliji-Fengxian deep seismic sounding profile

A deep seismic sounding profile in this paper, from Fuliji in Anhui Province to Fengxian of Shanghai City, is located at eastern China (Fig. 1). The field work was jointly accomplished by the Chinese Geological and Mineral Bureau, the China Seismological …     

Determination of omethoate by cathodically sweeping oscillopolarography

Determination of omethoate by cathodically sweeping oscillopolarography is described. The product of the alkaline hydrolysis exhibited a sensitive second derivative wave at −0.50 V (vs. SCE) in a 1.0 ×10⁻⁵mol/L sodium dodecylbenzene sulfonate (SDBS)+0.1 mol/L HAc-NaAc (pH 4.0) buffer. The peak current was linearly proportional to the concentration of omethoate in the range from 6.4×10⁻⁷ to 5.1×10⁻⁵ mol/L. The detection limit is 2.0×10⁻⁷ mol/L with the relative standard derivation (RSD) of 3.5%. The hydrolysis procedure and the electrode reaction were studied by voltammetry. Supported by the Foundation of Chinese-Franch Cooperation Programme on the Advanced Research Wang Yu: born in 1964. Lecturer. Cangzhou Teacher’s College, Cangzhou, Hebei, 061001     

Concentrations, profiles and gas-particle partitioning of PCDD/Fs, PCBs and PBDEs in the ambient air of an E-waste dismantling area, southeast China

Polychlorinated diebenzo-p-dioxins （PCDDs）, polychlorinated diebenzofurans （PCDFs）, polychlorinated biphenyls （PCBs） and polybrominated diphenyl ethers （PBDEs） were monitored in the ambient air of Taizhou, an E-waste dismantling area of southeast China to evaluate their concentrations, profiles and gas-particle partitioning. The ∑PCDD/Fs concentrations ranged from 2.91 to 50.6 pg/ma, with an average of 14.3 pg/ma. The I-TEQs for PCDD/Fs were in the range of 0.20-3.45 pg/ma, with an average of 1.10 pg/ma, The ∑PCBs concentrations and TEQs ranged from 4.23 to 11.35 ng/ma, 0.050 to 0.859 pg（TEQ）/ma, respectively. The concentrations of ∑PBDEs ranged from 92 to 3086 pg/ma, with an average of 894 pg/ma, The pollution levels of PCDD/Fs, PCBs and PBDEs were higher than other urban sites, which may be associated with the E-waste dismantling activities. The PCDD/Fs were found exclusively in the particle phase whereas PCBs distributed dominantly in the gas phase. The gas-partilce partitioning was also assessed by correlating the gas-particle partition coefficient （Kp） with the subcooled liquid vapor pressure （pL^0）. The measured particulate sorptions of PCDD/Fs, PCBs and PBDEs were compared with the predictions from Junge-Pankow model and Koa absorption model. The Junge-Pankow model well estimated the particulate fractions of PCBs. However, it underestimated the sorptions of PCDD/Fs and overestimated the fractions of PBDEs. The predicted particulate fractions of PCDD/Fs and PCBs from Koa model fitted well with the measured data.     

An infrared ring around the magnetar SGR 1900+14

Magnetars are a special class of slowly rotating (period approximately 5-12 s) neutron stars with extremely strong magnetic fields (>10(14 )G)--at least an order of magnitude larger than those of the 'normal' radio pulsars. The potential evolutionary links and differences between these two types of object are still unknown; recent studies, however, have provided circumstantial evidence connecting magnetars with very massive progenitor stars. Here we report the discovery of an infrared elliptical ring or shell surrounding the magnetar SGR 1900+14. The appearance and energetics of the ring are difficult to interpret within the framework of the progenitor's stellar mass loss or the subsequent evolution of the supernova remnant. We suggest instead that a dust-free cavity was produced in the magnetar environment by the giant flare emitted by the source in August 1998. Considering the total energy released in the flare, the theoretical dust-destruction radius matches well with the observed dimensions of the ring. We conclude that SGR 1900+14 is unambiguously associated with a cluster of massive stars, thereby solidifying the link between magnetars and massive stars.