排序方式： 共有115条查询结果，搜索用时 31 毫秒
11.
H. R. Merrett K. Kuijken M. R. Merrifield A. J. Romanowsky N. G. Douglas N. R. Napolitano M. Arnaboldi M. Capaccioli K. C. Freeman O. Gerhard N. W. Evans M. I. Wilkinson C. Halliday T. J. Bridges D. Carter 《Monthly notices of the Royal Astronomical Society》2003,346(4):L62-L66
We present a possible orbit for the Southern Stream of stars in M31, which connects it to the Northern Spur. Support for this model comes from the dynamics of planetary nebulae (PNe) in the disc of M31: analysis of a new sample of 2611 PNe obtained using the Planetary Nebula Spectrograph reveals ∼20 objects with kinematics inconsistent with the normal components of the galaxy, but which lie at the right positions and velocities to connect the two photometric features via this orbit. The satellite galaxy M32 is coincident with the stream both in position and velocity, adding weight to the hypothesis that the stream comprises its tidal debris. 相似文献
12.
E. Athanassoula Rachael Lynn Beaton 《Monthly notices of the Royal Astronomical Society》2006,370(3):1499-1512
The inclination of M31 is too close to edge-on for a bar component to be easily recognized and is not sufficiently edge-on for a boxy/peanut bulge to protrude clearly out of the equatorial plane. Nevertheless, a sufficient number of clues allow us to argue that this galaxy is barred. We use fully self-consistent N -body simulations of barred galaxies and compare them with both photometric and kinematic observational data for M31. In particular, we rely on the near-infrared photometry presented in a companion paper. We compare isodensity contours to isophotal contours and the light profile along cuts parallel to the galaxy major axis and offset towards the north, or the south, to mass profiles along similar cuts on the model. All these comparisons, as well as position–velocity diagrams for the gaseous component, give us strong arguments that M31 is barred. We compare four fiducial N -body models to the data and thus set constraints on the parameters of the M31 bar, as its strength, length and orientation. Our 'best' models, although not meant to be exact models of M31, reproduce in a very satisfactory way the main relevant observations. We present arguments that M31 has both a classical and a boxy/peanut bulge. Its pseudo-ring-like structure at roughly 50 arcmin is near the outer Lindblad resonance of the bar and could thus be an outer ring, as often observed in barred galaxies. The shape of the isophotes also argues that the vertically thin part of the M31 bar extends considerably further out than its boxy bulge, that is, that the boxy bulge is only part of the bar, thus confirming predictions from orbital structure studies and from previous N -body simulations. It seems very likely that the backbone of M31's boxy bulge is families of periodic orbits, members of the x1 -tree and bifurcating from the x1 family at its higher order vertical resonances, such as the x1v3 or x1v4 families. 相似文献
13.
KSS 31海洋重力仪配套接口子系统开发 总被引：1，自引：0，他引：1
介绍一种采用VC 语言开发成功的KSS 31型海洋重力仪导航系统适配的接口应用程序，对如何解决引进新型号设备与现有的系统(设备)集成(连接)问题有一定的借鉴作用。 相似文献
14.
Noel Cressie 《Mathematical Geology》1985,17(7):693-702
The relative variogram has been employed as a tool for correcting a simple kind of nonstationarity, namely that in which local variance is proportional to local mean squared. In the past, this has been linked in a vague way to the lognormal distribution, although if {Zt; t D}is strongly stationary and normal over a domain D,then clearly {exp (Zt); t D}will stillbe stationary, but lognormal. The appropriate link is made in this article through a universal transformation principle. More general situations are considered, leading to the use of a scaled variogram. 相似文献
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16.
S. T. Gottesman J. H. HunterJr V. Boonyasait 《Monthly notices of the Royal Astronomical Society》2002,337(1):34-40
Recent work by several groups has established the properties of the dwarf satellites to M31. We reexamine the reported kinematics of this group employing a fresh technique we have developed previously. By calculating the distribution of a χ statistic (which we define in the paper) for the M31 system, we conclude that the total mass (disc plus halo) of the primary is unlikely to be as great as that of our own Milky Way. In fact the χ distribution for M31 indicates that, like NGC 3992, it does not have a massive halo. In contrast, the analysis of the satellites of NGC 1961 and NGC 5084 provides strong evidence for massive haloes surrounding both spiral galaxies. 相似文献
17.
Douglas O. ReVelle 《Earth, Moon, and Planets》2008,102(1-4):345-356
We have developed a new approach to modeling the acoustic-gravity wave (AGW) radiation from bolide sources. This first effort
involves entry modeling of bolide sources that have available satellite data through procedures developed in ReVelle (Earth
Moon Planets 95, 441–476, 2004a; in: A. Milani, G. Valsecchi, D. Vokrouhlicky (eds) NEO Fireball Diversity: Energetics-based Entry Modeling and Analysis Techniques, Near-earth Objects: Our Celestial Neighbors
(IAU S236), 2007b). Results from the entry modeling are directly coupled to AGW production through line source blast wave theory for the initial
wave amplitude and period at (at 10 blast wave radii and perpendicular to the trajectory). The second effort involves the prediction of the formation
and or dominance of the propagation of the atmospheric Lamb, edge-wave composite mode in a viscous fluid (Pierce, J. Acoust.
Soc. Amer. 35, 1798–1807, 1963) as a function of the source energy, horizontal range and source altitude using the Lamb wave frequency that was deduced
directly during the entry modeling and that is used as a surrogate for the source energy. We have also determined that Lamb
wave production by bolides at close range decreases dramatically as either the source energy decreases or the source altitude
increases. Finally using procedures in Gill (Atmospheric-Ocean Dynamics, 1982) and in Tolstoy (Wave Propagation, 1973), we have analyzed two simple dispersion relationships and have calculated the expected dispersion for the Lamb edge-wave
mode and for the excited, propagating internal acoustic waves. Finally, we have used the above formalism to fully evaluate
these techniques for four large bolides, namely: the Tunguska bolide of June 30, 1908; the Revelstoke bolide of March 31,
1965; the Crete bolide of June 6, 2002 and the Antarctic bolide of September 3, 2004. Due to page limitations, we will only
present results in detail for the Revelstoke bolide. 相似文献
18.
Jun Ma ;Richard de Grijs ;Zhou Fan ;Soo-Chang Rey ;Zhen-Yu Wu ;Xu Zhou ;Jiang-Hua Wu ;Zhao-Ji Jiang ;Jian-Sheng Chen ;Kyungsook Lee ;Sangmo Tony Sohn 《天体物理学报》2009,(6):641-652
Mayall Ⅱ = G1 is one of the most luminous globular clusters （GCs） in M31. Here, we determine its age and mass by comparing multicolor photometry with theoretical stellar population synthesis models. Based on far- and near-ultraviolet GALEX photometry, broad-band UBVRI, and infrared JHKs 2MASS data, we construct the most extensive spectral energy distribution of G 1 to date, spanning the wavelength range from 1538 to 20 000A. A quantitative comparison with a variety of simple stellar population （SSP） models yields a mean age which is consistent with G1 being among the oldest building blocks of M31 and having formed within ～1.7 Gyr after the Big Bang. Irrespective of the SSP model or stellar initial mass function adopted, the resulting mass estimates （of order 10^7M⊙） indicate that GI is one of the most massive GCs in the Local Group. However, we speculate that the cluster＇s exceptionally high mass suggests that it may not be a genuine GC. Our results also suggest that G1 may contain, on average, （1.65±0.63） × 10^2L⊙ far-ultraviolet-bright, hot, extreme horizontal-branch stars, depending on the adopted SSP model. In addition, we demonstrate that extensive multi-passband photometry coupled with SSP analysis enables one to obtain age estimates for old SSPs that have similar accuracies as those from integrated spectroscopy or resolved stellar photometry, provided that some of the free parameters can be constrained independently. 相似文献
19.
针对中国业务中期数值预报模式T213对中雨量级以上的降水预报空报比较明显的问题,文中对此模式预报的降水进行了诊断分析。发现T213模式预报的总降水分布主要是由可分辨尺度降水决定的,且在降水偏多最明显的地区,可分辨尺度的降水即超过或达到了观测的总降水,表明降水空报的主要原因在于可分辨尺度降水偏多。可分辨尺度降水偏多的可能原因有：土壤湿度初始化、云变量的初始化和直接产生降水的云与对流参数化方案存在一定的缺陷。鉴于前两者是目前国际上的难点,文中针对第3个方面的可能原因进行了分析和相应的改进。包括在对流方案之前增加一次云方案的调用;对流参数化方案的闭合由“动力型”改为对流有效位能调整闭合;更复杂的对流触发机制;改进冰沉降和降水通量计算。改进的主要目的是使对流参数化方案更活跃,从而减少格点尺度对流的发生。采用改进的方案,进行了敏感性试验和2005年夏季的连续滚动同化预报试验,并与中国区域400个标准站的降水观测和GPCP的全球降水观测进行了比较。结果表明,改进的方案无论是对中国区域还是全球夏季平均的降水分布预报都好于业务,但四川省和赤道东太平洋降水偏多的问题依然存在。中国区域的降水统计检验还表明,除小雨外,其他量级在大部分时效上降水的TS评分增加,预报偏差降低。 相似文献
20.
分析了2005年5月11日至6月10日的NCEP-FNL与T213L31分析资料在位势高度、温度和风场上的整体差异,揭示了低层差异最小,差异极值主要分布在3个关键区的特征。进一步通过地形高度差异与位势高度差异的相关性分析,认为青藏高原附近的地形高度差异的极值是引起两种资料位势高度差异的主要原因,并计算分析了这种差异对高原周围中低层大气环流的动力和热力影响。结果显示,在NCEP-FNL中的西南涡强度和热源作用较强,中层风速切变较弱。 相似文献