流动重力布局评价及其观测技术     

石亚雄  项爱民 《大地测量与地球动力学》1994,(3)

本文从流动重力测量的布局、复测周期以及观测技术等方面介绍了地震系统重力测量的现状，提出了优化现行布局、调整复测周期、提高观测技术以及改善观测条件的具体意见。指出：为了获得与地震有关的重力变化信息，当前的重点应放在布局的优化和复测周期的调整上。  相似文献   

南极纳尔逊冰帽的雪层及其成冰作用研究          下载免费PDF全文

王晓军  秦大河  刘琛  钱嵩林 《极地研究》1990,2(2):13-21

纳尔逊冰帽雪—粒雪的演化依赖于融水渗浸冻结作用下的暖变质过程。积雪的密实化过程的快慢,取决于温度条件和融水的参与程度,以及自身的物理状况。粒雪的密实化过程表现为均匀且变幅小。纳尔逊冰帽成冰深度在23～25m,成冰历时17～19年。成冰带分为暖渗浸—重结晶带,渗浸—冻结带,消融带。  相似文献   

Distribution of the nonlinear random ocean wave period     

侯一筠  李明杰  宋贵霆  司广成  齐鹏  胡珀 《中国海洋湖沼学报》2009,27(4):919-923

Because of the intrinsic difficulty in determining distributions for wave periods, previous studies on wave period distribution models have not taken nonlinearity into account and have not performed well in terms of describing and statistically analyzing the probability density distribution of ocean waves. In this study, a statistical model of random waves is developed using Stokes wave theory of water wave dynamics. In addition, a new nonlinear probability distribution function for the wave period is presented with the parameters of spectral density width and nonlinear wave steepness, which is more reasonable as a physical mechanism. The magnitude of wave steepness determines the intensity of the nonlinear effect, while the spectral width only changes the energy distribution. The wave steepness is found to be an important parameter in terms of not only dynamics but also statistics. The value of wave steepness reflects the degree that the wave period distribution skews from the Cauchy distribution, and it also describes the variation in the distribution function, which resembles that of the wave surface elevation distribution and wave height distribution. We found that the distribution curves skew leftward and upward as the wave steepness increases. The wave period observations for the SZFII-1 buoy, made off the coast of Weihai (37°27.6′ N, 122°15.1′ E), China, are used to verify the new distribution. The coefficient of the correlation between the new distribution and the buoy data at different spectral widths (ν=0.3−0.5) is within the range of 0.968 6 to 0.991 7. In addition, the Longuet-Higgins (1975) and Sun (1988) distributions and the new distribution presented in this work are compared. The validations and comparisons indicate that the new nonlinear probability density distribution fits the buoy measurements better than the Longuet-Higgins and Sun distributions do. We believe that adoption of the new wave period distribution would improve traditional statistical wave theory.  相似文献   

The angular momentum content of dwarf galaxies: new challenges for the theory of galaxy formation     

Frank C. van den Bosch  reas Burkert  Rob A. Swaters 《Monthly notices of the Royal Astronomical Society》2001,326(3):1205-1215

We compute the specific angular momentum distributions for a sample of low-mass disc galaxies observed by Swaters. We compare these distributions to those of dark matter haloes obtained by Bullock et al. from high-resolution N -body simulations of structure formation in a ΛCDM universe. We find that although the disc mass fractions are significantly smaller than the universal baryon fraction, the total specific angular momenta of the discs are in good agreement with those of dark matter haloes. This suggests that discs form out of only a small fraction of the available baryons, but yet manage to draw most of the available angular momentum. In addition we find that the angular momentum distributions of discs are clearly distinct from those of the dark matter; discs lack predominantly both low and high specific angular momenta. Understanding these findings in terms of a coherent picture for disc formation is challenging. Cooling, feedback and stripping, which are the main mechanisms to explain the small disc mass fractions found, seem unable to simultaneously explain the angular momentum distributions of the discs. In fact, it seems that the baryons that make up the discs must have been born out of angular momentum distributions that are clearly distinct from those of ΛCDM haloes. However, the dark and baryonic mass components experience the same tidal forces, and it is therefore expected that they should have similar angular momentum distributions. Therefore, understanding the angular momentum content of disc galaxies remains an important challenge for our picture of galaxy formation.  相似文献   

恒星形成区GGD12-15的近红外观测     

房敏  姚永强 《天文学报》2004,45(1):1-15

给出恒星形成区GGD12-15的宽波段JHK和窄波段H2v=1-0S(1)近红外成像观测．观测图像揭示了致密的年轻红外星团和与红外源成协的红外星云，并发现了以H2发射结表征的星团外流活动．大多数红外点源在光学波段不可见；对76颗红外点源的JHK′测光结果显示，有32颗具有红外超，其中5颗表现原恒星特征，表明分子云中的恒星形成活动很活跃．以B8光谱型作为大质量星分界，由色星等图估计出大质量星所占星团比例为-10％～26％．GGD12—15星团的K′星等分布的峰值位于15.0mag，并在13．0mag-16．0mag平坦分布；[H—K′]色分布的峰值出现在-0．7mag，在此以上更红的星团成分占70％．在GGD12-15区新发现的氢分子发射结集中在星团中心领域，其空间分布明显与剧烈的恒星形成活动相关；有5个发射结位于分子外流的中心区域，暗示其激发可能与分子外流同源．  相似文献   

The K-band galaxy luminosity functions of three massive high-redshift clusters of galaxies     

S. C. Ellis  L. R. Jones 《Monthly notices of the Royal Astronomical Society》2004,348(1):165-175

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The gravitational wave background from neutron star birth throughout the cosmos     

E. Howell  D. Coward  R. Burman  D. Blair  J. Gilmore 《Monthly notices of the Royal Astronomical Society》2004,351(4):1237-1246

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New OH masers at 13 441 MHz     

J. L. Caswell 《Monthly notices of the Royal Astronomical Society》2004,352(1):101-111

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Disk Planet Interactions And Early Evolution in Young Planetary Systems     

J. C. B. Papaloizou 《Celestial Mechanics and Dynamical Astronomy》2005,91(1-2):33-57

We study and review disk protoplanet interactions using local shearing box simulations. These suffer the disadvantage of having potential artefacts arising from periodic boundary conditions but the advantage, when compared to global simulations, of being able to capture much of the dynamics close to the protoplanet at high resolution for low computational cost. Cases with and without self sustained MHD turbulence are considered. The conditions for gap formation and the transition from type I migration are investigated and found to depend on whether the single parameter M _p R ³/(M_* H ³), with M _p, M_*, R, and H being the protoplanet mass, the central mass, the orbital radius and the disk semi-thickness, respectively, exceeds a number of order unity. We also investigate the coorbital torques experienced by a moving protoplanet in an inviscid disk. This is done by demonstrating the equivalence of the problem for a moving protoplanet to one where the protoplanet is in a fixed orbit which the disk material flows through radially as a result of the action of an appropriate external torque. For sustainable coorbital torques to be realized a quasi steady state must be realized in which the planet migrates through the disk without accreting significant mass. In that case, although there is sensitivity to computational parameters, in agreement with earlier work by Masset and Papaloizou [2003, ApJ, 588, 494] based on global simulations, the coorbital torques are proportional to the migration speed and result in a positive feedback on the migration, enhancing it and potentially leading to a runaway. This could lead to fast migration for protoplanets in the Saturn mass range in massive disks and may be relevant to the mass period correlation for extrasolar planets which gives a preponderance of sub Jovian masses at short orbital periods.  相似文献   

Smoothed Particle Magnetohydrodynamics – III. Multidimensional tests and the  ∇·B= 0  constraint     

D. J. Price  J. J. Monaghan 《Monthly notices of the Royal Astronomical Society》2005,364(2):384-406

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