Orbital resonance in a dissipative medium     

Richard Greenberg 《Icarus》1978,33(1):62-73

Orbital resonances tend to force bodies into noncircular orbits. If a body is also under the influence of an eccentricity-reducing medium, it will experience a secular change in semimajor axis which may be positive or negative depending on whether its orbit is exterior or interior to that of the perturbing body. Thus a dissipative medium can promote either a loss or a gain in orbital energy. This process may explain the resonant structure of the asteroid belt and of Saturn's rings. For reasonable early solar system parameters, it would clear a gap near the 2:1 resonance with Jupiter on a time scale of a few thousand years; the gap width would be comparable to the Kirkwood gap presently at the location in the asteroid belt. Similarly, a gap comparable in width to Cassini's division would be cleared in Saturn's rings at the 2:1 resonance with Mimas in ～10⁶ yr. Most of the material from the gap would be deposited at the outer edge of ring B. The process would also affect the radial distribution of preplanetary material. Moreover, it provides an explanation for the large amplitude of the Titan-Hyperion libration. Consideration of the effects of dissipation on orbits near the stable L₄ and L₅ points of the restricted three-body problem indicates that energy loss causes particles to move away from these points. This results explains the large amplitude of Trojan asteroids about these points and the possible capture of Trojan into orbit about Jupiter.  相似文献   

Size distribution of particles in planetary rings     

Richard Greenberg  Donald R. Davis  William K. Hartmann  Clark R. Chapman 《Icarus》1977,30(4):769-779

Harris (Icarus24, 190–192) has suggested that the maximum size of particles in a planetary ring is controlled by collisional fragmentation rather than by tidal stress. While this conclusion is probably true, estimated radius limits must be revised upward from Harris' values of a few kilometers by at least an order of magnitude. Accretion of particles within Roche's limit is also possible. These considerations affect theories concerning the evolution of Saturn's rings, of the Moon, and of possible former satellites of Mercury and Venus. In the case of Saturn's rings, comparison of various theoretical scenarios with available observational evidence suggests that the rings formed from the breakup of larger particles rather than from original condensation as small particles. This process implies a distribution of particle sizes in Saturn's rings possibly ranging up to ～100 km but with most cross-section in cm-scale particles.  相似文献   

The effect of sub-pixel slope variations on photoclinometry     

Richard Greenberg  Marita Morris 《Icarus》2011,214(1):348-350

Sub-pixel slope variations can have significant effects on the intensity of light scattered from a planetary surface. As a result, determination of the surface slope from the apparent brightness of a given pixel can be confounded by uncertainly in such variations. Under a wide range of conditions, the average slope across the pixel may be different from what is inferred by photoclinometry. Because topography is derived from photoclinometry by integrating the slope across an image composed of many pixels, topographic elevation could in principle be distorted considerably by this effect. As actually applied, photoclinometry generally includes strategies designed to mitigate these effects substantially. Nevertheless, the potential always exists for unknown variations in the character of sub-pixel topography (among other uncertainties such as albedo variations) to introduce errors. The results shown here show the importance of the mitigating strategies and of considering the magnitude of uncertainties in determination of topography.  相似文献   

新疆阿尔泰铁木尔特铅锌矿床流体包裹体研究及地质意义   总被引：6，自引：3，他引：3  

耿新霞  杨富全  杨建民  黄承科  刘锋  柴凤梅  张志欣 《岩石学报》2010,26(3):695-706

铁木尔特中型铅锌矿是阿尔泰山南缘克兰盆地内的重要VMS型矿床。矿床赋存于上志留统-下泥盆统康布铁堡组上亚组第二岩性段,容矿岩石为大理岩、绿泥石英片岩、变钙质粉砂岩、夕卡岩。矿体呈似层状和透镜状。矿床的形成经历了喷流沉积期、叠加改造期和表生期。石英、长石、方解石和石榴子石中包裹体类型主要为液体包裹体,在石英中另出现了气体包裹体、纯气体包裹体、含子矿物多相包裹体、含液体CO2的三相包裹体和两相CO2包裹体。喷流沉积期成矿流体均一温度变化于150～330℃,其峰值是165℃和285℃,成矿流体盐度(NaCleq)为4%～16%,流体密度为0.77～0.97g/cm3,流体阳离子主要以Na+为主,次之为K+,阴离子以Cl-为主,其次是SO42-,气相成分主要是H2O和CO2。叠加改造期均一温度范围是150～480℃,峰值为285℃,盐度(NaCleq)为2.2%～17.08%和33.93%～47.2%,流体密度变化于0.61～1.03g/cm3之间,流体阳离子主要以Na+为主,次为K+、Mg2+、Ca2+,阴离子以Cl-为主,其次是SO42-,气相成分主要是H2O和CO2,其次为N2、CH4,含有少量C2H6。  相似文献   

Craters on asteroids: Reconciling diverse impact records with a common impacting population     

David P. O'Brien  Richard Greenberg 《Icarus》2006,183(1):79-92

O'Brien and Greenberg [O'Brien, D.P., Greenberg, R., 2005. Icarus 178, 179-212] developed a self-consistent numerical model of the collisional and dynamical evolution of the main-belt and NEA populations that was tested against a diverse range of observational and theoretical constraints. In this paper, we use those results to update the asteroid cratering model of Greenberg et al. [Greenberg, R., Nolan, M.C., Bottke, W.F., Kolvoord, R.A., Veverka, J., 1994. Icarus 107, 84-97; Greenberg, R., Bottke, W.F., Nolan, M., Geissler, P., Petit, J., Durda, D.D., Asphaug, E., Head, J., 1996. Icarus 120, 106-118], and show that the main-belt asteroid population from the O'Brien and Greenberg collisional/dynamical evolution modeling is consistent with the crater records on Gaspra, Ida, Mathilde, and Eros, the four asteroids that have been observed by spacecraft.  相似文献   

Modelling the astronomical silicate features – I. On the spectrum subtraction method     

Aigen Li  J. Mayo Greenberg  Gang Zhao 《Monthly notices of the Royal Astronomical Society》2002,334(4):840-846

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A Melt-through Model for Chaos Formation on Europa   总被引：1，自引：0，他引：1  

David P. O'BrienPaul Geissler  Richard Greenberg 《Icarus》2002,156(1):152-161

The character of chaotic terrain on Europa is consistent with its formation by the melting of a thin conducting ice shell from below. Tidal dissipation can provide adequate energy for such a process. For example, only a few percent of Europa's predicted tidal heat, spread over a region 200 km in diameter, can lead to large melt regions within a few tens of thousands of years. Stronger, more localized concentrations result in melt-through in significantly shorter times (i.e., a few hundred years). The time scale for melt-through is shorter than the time scale for the solid-state viscous inflow of ice by several orders of magnitude. In general, modest concentrations of tidal heat can melt ice away faster than viscous inflow, leading to melt-through. A mechanism to transmit these heat concentrations through the ocean is required for this model. Such heat transport could be the result of convective plumes in the ocean driven by seafloor volcanism or by the destabilization of a stratified ocean.  相似文献   

Characterizing multi-planet systems with classical secular theory     

Christa Van Laerhoven  Richard Greenberg 《Celestial Mechanics and Dynamical Astronomy》2012,113(2):215-234

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Three‐dimensional textural and compositional analysis of particle tracks and fragmentation history in aerogel     

Denton S. Ebel  Michael Greenberg  Mark L. Rivers  Matthew Newville 《Meteoritics & planetary science》2009,44(10):1445-1463

Abstract— We report analyses of aerogel tracks using (1) synchrotron X‐ray computed microtomography (XRCMT), (2) laser confocal scanning microscopy (LCSM), and (3) synchrotron radiation X‐ray fluorescence (SRXRF) of particles and their paths resulting from simulated hypervelocity impacts (1–2), and a single ～1 mm aerogel track from the Stardust cometary sample collector (1–3). Large aerogel pieces can be imaged sequentially, resulting in high spatial resolution images spanning many tomographic fields of view (‘lambda‐tomography’). We report calculations of energy deposited, and tests on aromatic hydrocarbons showing no alteration in tomography experiments. Imaging at resolutions from ～17 to ～1 micron/pixel edge (XRCMT) and to <100 nm/pixel edge (LCSM) illustrates track geometry and interaction of particles with aerogel, including rifling, particle fragmentation, and final particle location. We present a 3‐D deconvolution method using an estimated point‐spread function for aerogel, allowing basic corrections of LCSM data for axial distortion. LCSM allows rapid, comprehensive, non‐destructive, high information return analysis of tracks in aerogel keystones, prior to destructive grain extraction. SRXRF with LCSM allows spatial correlation of grain size, chemical, and mineralogical data. If optical methods are precluded in future aerogel capture missions, XRCMT is a viable 3D imaging technique. Combinations of these methods allow for complete, nondestructive, quantitative 3‐D analysis of captured materials at high spatial resolution. This data is fundamental to understanding the hypervelocity particle‐aerogel interaction histories of Stardust grains.  相似文献   

A numerical model investigation of tidal phenomena in the Bay of Fundy and Gulf of Maine     

David A. Greenberg 《Marine Geodesy》2013,36(2):161-187

A numerical model is developed to examine tidal properties of the Bay of Fundy and Gulf of Maine. The model is run with a pure M₂ tidal input on the open boundary, and calibrated by adjusting the friction coefficient to achieve good agreement with inshore observations. An examination of aspects of the tidal regime is made, with particular attention paid to the upper reaches of the bay. Mean energy and work values are computed. The fundamental period of the system is estimated. The effects of tidal power plants on the tidal regime are examined.  相似文献