基于移动网络的端到端密钥协商协议

虽然3G网络的安全机制扩展到核心网络,但是并没有实现端到端安全.基于自生成证书公钥密码体制,设计一种端到端密钥协商协议,只需要一个消息交换就可以建立安全的三方会话密钥.安全性分析结果表明:基于移动网络的端到端密钥协商协议能够解决密钥管理及第三方无举证窃听,与其他密钥协商协议相比,具有较好的安全性,为端到端加密在移动通信系统中的大规模应用提供基础.     

关联指数误差和样本容量

根据关联指数的定义，推导了ＧＰ法计算关联指数时的观测数据误差与关联指数误差的关系，导出了任意两个嵌入空间维上关联指数之差的表达式，并提出了一种确定样本容量限的方法。     

3G智能手机在地震监测预报工作中的应用

结合3G智能手机小巧易携带、可随时随地上网,配备先进的软硬件系统,可根据需要开发、安装应用软件,功能越来越强大等优点,以中兴U880为例,介绍3G智能手机存地震监测预报工作中的实际应用。     

Surface motion in the pulsating DA white dwarf G29‐38

We present time-resolved spectrophotometry of the pulsating DA white dwarf G29-38. As in previous broad-band photometry, the light curve shows the presence of a large number of periodicities. Many of these are combination frequencies, i.e. periodicities occurring at frequencies that are sums or differences of frequencies of stronger, real modes. We identify at least six real modes, and at least five combination frequencies. We measure line-of-sight velocities for our spectra and detect periodic variations at the frequencies of five of the six real modes, with amplitudes of up to 5 km s⁻¹. We argue that these variations reflect the horizontal surface motion associated with the g-mode pulsations. No velocity signals are detected at any of the combination frequencies, confirming that the flux variations at these frequencies do not reflect physical pulsation, but rather reflect mixing of frequencies owing to a non-linear transformation in the outer layers of the star. We discuss the amplitude ratios and phase differences found for the velocity and light variations, as well as those found for the real modes and their combination frequencies, both in a model-independent way and in the context of models based on the convective-driving mechanism. In a companion paper, we use the wavelength dependence of the amplitudes of the modes to infer their spherical degree.     

Subarcsec 10μm imaging of bipolar flow sources

We have started a program of high-resolution (0.4/pixel) 10m imaging of bipolar outflow sources using the 10m camera CAMIRAS. We present recent results obtained at the Canada France Hawaii Telescope which reveal extended emission or IR companions in several luminous objects. The extended emission we detected probably arises from transiently heated very small grains, while the newly discovered companions could contribute significantly to the outflow activity and extended far-IR emission usually attributed to the main optical source.     

2种江蓠藻体切段的再生

初步研究了细基江蓠繁枝变种（Ｇ． ｔｅｎｕｉｓｔｉｐｉｔａｔａ ｖａｒ． ｌｉｕｉ）和细基江蓠（Ｇ． ｔｅｎｕｉｓｔｉｐｉｔａｔａ）切段培养的适宜培养基及其切段的再生特点。在此基础上,还研究了几种植物生长调节剂对江蓠藻体切段再生的影响。研究表明,江蓠藻体在改良ＰＥＳ培养基中生长良好。两种藻体的外皮层细胞均可产生长成新枝的生长点,并且表现出相同的再生极性。无论细基江蓠繁枝变种还是细基江蓠的切段都是在形态学上端切口处产生新枝,下端不再生;带分枝的切段,其分枝断口处亦可再生新枝。适宜的植物生长调节剂可明显促进藻体芽的产生和生长。１ ｍ ｇ／ ＬＢＡ 明显促进细基江蓠繁枝变种切段的再生,２ ｍ ｇ／ Ｌ ＢＡ＋ ０．５ ｍ ｇ／Ｌ ＮＡＡ 显著促进细基江蓠切段的再生     

Characteristics of the supernova remnant G351.7+0.8 and a distance argument against its association with PSR J1721−3532

New images of the supernova remnant (SNR) G351.7+0.8 are presented based on 21-cm H  i -line emission and continuum emission data from the Southern Galactic Plane Survey. SNR G351.7+0.8 has a flux density of 8.4 ± 0.7 Jy at 1420 MHz. Its spectral index is 0.52 ± 0.25 ( S = v ^−α) between 1420 and 843 MHz, typical of adiabatically expanding shell-like remnants. H  i observations show structures possibly associated with the SNR in the radial velocity range of −10 to −18 km s⁻¹, and suggest a distance of 13.2 kpc and a radius of 30.7 pc. The estimated Sedov age for G351.7+0.8 is less than  6.8×10⁴ yr  . A young radio pulsar PSR J1721−3532 lies close to SNR G351.7+0.8 on the sky. The new distance and age of G351.7+0.8 and recent proper motion measurements of the pulsar strongly argue against an association between SNR G351.7+0.8 and PSR J1721−3532. There is an unidentified, faint X-ray point source 1RXS J172055.3−353937 which is close to G351.7+0.8. This may be a neutron star potentially associated with G351.7+0.8.     

CO Clouds around SNR G21.8-0.6 and G32.8-0.1

We made the first CO(I—0) mapping to SNR G21.8-0.6 and SNR G32.8-0.1, both associated with OH 1720 MHz maser.Based on the morphological correspondence and velocity and position agreement between the radio remnant and the CO clouds,we tentatively identify the clouds that are respectively interacting with the two SNRs.     

利用空间测地技术结果估计地球平均下地幔粘性(英)

基于IEC－4G冰期后地壳反弹模型,和地球上Laurentia,Fennoscandia,Antarctica,andGreenland四大冰盖最近21000年以来的冰融参数,计算了对地球最大主转动惯量的影响△I33,并进而由现代空间测地技术观测资料分析得到的地球自转非潮汐加速项为约束,估计了地球平均下地幔（670km以下）粘性vLM为（0．9～2．5）·1022Pas,这个结果表明了vLM应具有1022Pas量级．     

Evidence for the stratification of Fe in the photosphere of G191-B2B

The presence of heavy elements in the atmospheres of the hottest H-rich DA white dwarfs has been the subject of considerable interest. While theoretical calculations can demonstrate that radiative forces, counteracting the effects of gravitational settling, can explain the detections of individual species, the predicted abundances do not accord well with observation. However, accurate abundance measurements can only be based on a thorough understanding of the physical structure of the white dwarf photospheres, which has proved elusive. Recently, the availability of new non-local thermodynamic equilibrium model atmospheres with improved atomic data has allowed self-consistent analysis of the extreme ultraviolet (EUV), far UV and optical spectra of the prototypical object G191-B2B. Even so, the predicted and observed stellar fluxes remain in serious disagreement at the shortest wavelengths (below ≈190 Å), while the inferred abundances remain largely unaltered. We show here that the complete spectrum of G191-B2B can be explained by a model atmosphere where Fe is stratified, with increasing abundance at greater depth. This abundance profile may explain the difficulties in matching observed photospheric abundances, usually obtained by analyses using homogeneous model atmospheres, to the detailed radiative levitation predictions, particularly as the latter are only strictly valid for regions deeper than where the EUV/far UV lines and continua are formed. Furthermore, the relative depletion of Fe in the outer layers of the atmosphere may be evidence for radiatively driven mass-loss in G191-B2B.