扰动重力梯度的非奇异表示   总被引：5，自引：0，他引：5  

刘晓刚  吴晓平  赵东明  吴星 《测绘学报》2010,39(5):450-457

在局部指北坐标系中用地心球坐标来表示扰动重力梯度张量,当计算点趋近于两极时,由于Legendre函数的一阶和二阶导数以及分母上所含余纬的正弦函数,将导致扰动重力梯度张量的计算出现无穷大。因此,本文引入了Legendre函数的一阶和二阶导数以及 无奇异性的计算公式,并且进一步推导了 无奇异性的计算公式。在将Legendre函数的一阶和二阶导数以及 、 无奇异性的计算公式代入到扰动重力梯度张量各分量的求解中时,又充分考虑了m等于0,1,2以及其它量时的复杂情况,建立了扰动重力梯度张量各分量无奇异性的详细计算模型。通过模拟实验表明,本文所建立的详细计算模型不仅能够完全满足当前卫星重力梯度张量计算的精度要求,而且模型稳定、可靠、易于编程实现。  相似文献   

New mass formula for spherically symmetric stellar configurations     

U. Bleyer  L. Sh. Grigorian  R. M. Avakian  E. V. Chubarian 《Astronomische Nachrichten》1995,316(1):1-7

A new formula is derived for the mass of spherically symmetric stellar configurations. An expression will be given where the mass square is connected to an integral over the pressure of gravitating matter. This formula turns out to hold for Newtonian gravity, for Einstein's GRT, for projective and bimetric scalar-tensor and further theories of gravitation.  相似文献   

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周世昌  王庆宾  朱雷鸣 《大地测量与地球动力学》2009,29(1):88-90

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Detecting ionized bubbles in redshifted 21-cm maps     

Kanan K. Datta  Somnath Bharadwaj  T. Roy Choudhury 《Monthly notices of the Royal Astronomical Society》2007,382(2):809-818

Linear transient phenomena induced by flow non-normality in thin self-gravitating astrophysical discs are studied using the shearing sheet approximation. The considered system includes two modes of perturbations: vortex and (spiral density) wave. It is shown that self-gravity considerably alters the vortex mode dynamics; its transient (swing) growth may be several orders of magnitude stronger than in the non-self-gravitating case and two to three times larger than the transient growth of the wave mode. Based on this finding, we comment on the role of vortex mode perturbations in a gravitoturbulent state. We also describe the linear coupling of the perturbation modes, caused by the differential character of disc rotation. The coupling is asymmetric: vortex mode perturbations are able to excite wave mode perturbations, but not vice versa. This asymmetric coupling lends additional significance to the vortex mode as a participant in spiral density waves and shock manifestations in astrophysical discs.  相似文献   

Gravitational collapse in an expanding universe: scaling relations for two-dimensional collapse revisited     

Suryadeep Ray  J. S. Bagla  T. Padmanabhan 《Monthly notices of the Royal Astronomical Society》2005,360(2):546-554

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Neutrinos as cluster dark matter     

R. H. Sanders 《Monthly notices of the Royal Astronomical Society》2007,380(1):331-338

The dynamical mass of clusters of galaxies, calculated in terms of MOdified Newtonian Dynamics (MOND), is a factor of 2 or 3 times smaller than the Newtonian dynamical mass but remains significantly larger than the observed baryonic mass in the form of hot gas and stars in galaxies. Here I consider further the suggestion that the undetected matter might be in the form of cosmological neutrinos with mass of the order of 2 eV. If the neutrinos and baryons have comparable velocity dispersions and if the two components maintain their cosmological density ratio, then the electron density in the cores of clusters should be proportional to T ^3/2, as appears to be true in non-cooling flow clusters. This is equivalent to the 'entropy floor' proposed to explain the steepness of the observed luminosity–temperature relation, but here preheating of the medium is not required. Two-fluid (neutrino–baryon) hydrostatic models of clusters, in the context of MOND, reproduce the observed luminosity–temperature relation of clusters. If the β law is imposed on the gas density distribution, then the self-consistent models predict the general form of the observed temperature profile in both cooling and non-cooling flow clusters.  相似文献   

Modelling the Pioneer anomaly as modified inertia     

M. E. McCulloch 《Monthly notices of the Royal Astronomical Society》2007,376(1):338-342

This paper proposes an explanation for the Pioneer anomaly: an unexplained Sunward acceleration of 8.74 ± 1.33 × 10⁻¹⁰ m s⁻² seen in the behaviour of the Pioneer probes. Two hypotheses are made. (1) Inertia is a reaction to Unruh radiation and (2) this reaction is weaker for low accelerations because some wavelengths in the Unruh spectrum do not fit within a limiting scale (twice the Hubble distance) and are disallowed: a process similar to the Casimir effect. When these ideas are used to model the Pioneer crafts' trajectories, there is a slight reduction in their inertial mass, causing an anomalous Sunward acceleration of 6.9 ± 3.5 × 10⁻¹⁰ m s⁻² which agrees within error bars with the observed Pioneer anomaly beyond 10 au from the Sun. This new scheme is appealingly simple and does not require adjustable parameters. However, it also predicts an anomaly within 10 au of the Sun, which has not been observed. Various observational tests for the idea are proposed.  相似文献   

Non-Gaussian cosmic microwave background temperature fluctuations from peculiar velocities of clusters     

Naoki Yoshida †  Ravi K. Sheth  Antonaldo Diaferio 《Monthly notices of the Royal Astronomical Society》2001,328(2):669-677

We use numerical simulations of a (480 Mpc  h ⁻¹)³ volume to show that the distribution of peak heights in maps of the temperature fluctuations from the kinematic and thermal Sunyaev–Zeldovich (SZ) effects will be highly non-Gaussian, and very different from the peak-height distribution of a Gaussian random field. We then show that it is a good approximation to assume that each peak in either SZ effect is associated with one and only one dark matter halo. This allows us to use our knowledge of the properties of haloes to estimate the peak-height distributions. At fixed optical depth, the distribution of peak heights resulting from the kinematic effect is Gaussian, with a width that is approximately proportional to the optical depth; the non-Gaussianity comes from summing over a range of optical depths. The optical depth is an increasing function of halo mass and the distribution of halo speeds is Gaussian, with a dispersion that is approximately independent of halo mass. This means that observations of the kinematic effect can be used to put constraints on how the abundance of massive clusters evolves, and on the evolution of cluster velocities. The non-Gaussianity of the thermal effect, on the other hand, comes primarily from the fact that, on average, the effect is larger in more massive haloes, and the distribution of halo masses is highly non-Gaussian. We also show that because haloes of the same mass may have a range of density and velocity dispersion profiles, the relation between halo mass and the amplitude of the thermal effect is not deterministic, but has some scatter.  相似文献   

Separation Problem in Satellite Gravimetry     

SHEN Wenbin NING Jinsheng 《地球空间信息科学学报》2007,10(1):4-11

The problem of separating gravitation from inertia is discussed in very general sense, and the conclusion is positive: man can separate gravitation from inertia, if various observation techniques are applied for. The accelerometer's position problem in satellite gravimetry is investigated, and the additional acceleration effect due to the position error of an instrument as well as the difference between the mass center and the gravity center is explored.  相似文献   

Accuracy Analysis of Geopotential Coefficients Recovered from In-situ Disturbing Potential by Energy Conservation Method     

ZOU Xiancai LI Jiancheng LUO Jia XU Xinyu 《地球空间信息科学学报》2007,10(4):255-259

The characteristics of the normal equation created in recovering the Earth gravity model (EGM) by least-squares(LS) adjustment from the in-situ disturbing potential is discussed in detail. It can be co...  相似文献