The scattered disk as a source of Halley-type comets     

Harold F. Levison  Martin J. Duncan 《Icarus》2006,184(2):619-633

We investigate a new dynamical mechanism for producing Halley-type comets from the scattered disk of comets. Levison and Duncan [Levison, H., Duncan, M., 1997. Icarus 127, 13-32] and Duncan and Levison [Duncan, M., Levison, H., 1997. Science 276, 1670-1672] showed that a significant number of objects leave the scattered disk by evolving to semi-major axes greater than 1000 AU. We find that once these objects reach semi-major axes on the order of ¹⁰⁴ AU, a significant fraction immediately have their perihelia driven inward by the galactic tides. Approximately 0.01% of the objects that reach ¹⁰⁴ AU then evolve onto orbits similar to the observed Halley-like comets due to gravitational interactions with the giant planets. The orbital element distribution resulting from this process is statistically consistent with observations. We discuss the implications of this model for the number of objects in the scattered disk in the text. The model predicts a temporal variation in the influx of HTCs with a period of ∼118 Myr. At the peak, the model predicts that there should be roughly 10 times as many HTCs as currently observed (i.e., there should be weak HTC showers). However, the model may inflate the importance of these showers because it does not include the effects of passing stars and giant molecular clouds.  相似文献   

Petrology and origin of amoeboid olivine aggregates in CR chondrites     

Michael K. WEISBERG  Harold C. CONNOLLY  Denton S. EBEL 《Meteoritics & planetary science》2004,39(10):1741-1753

Abstract— Amoeboid olivine aggregates (AOAs) are irregularly shaped, fine‐grained aggregates of olivine and Ca, Al‐rich minerals and are important primitive components of CR chondrites. The AOAs in CR chondrites contain FeNi metal, and some AOAs contain Mn‐rich forsterite with up to 0.7 MnO and Mn:Fe ratios greater than one. Additionally, AOAs in the CR chondrites do not contain secondary phases (nepheline and fayalitic olivine) that are found in AOAs in some CV chondrites. The AOAs in CR chondrites record a complex petrogenetic history that included nebular gas‐solid condensation, reaction of minerals with the nebular gas, small degrees of melting, and sintering of the assemblage. A condensation origin for the Mn‐rich forsterite is proposed. The Mn‐rich forsterite found in IDPs, unequilibrated ordinary chondrite matrix, and AOAs in CR chondrites may have had a similar origin. A type A calcium, aluminum‐rich inclusion (CAI) with an AOA attached to its Wark‐Lovering rim is also described. This discovery reveals a temporal relationship between AOAs and type A inclusions. Additionally, a thin layer of forsterite is present as part of the Wark‐Lovering rim, revealing the crystallization of olivine at the end stages of Wark‐Lovering rim formation. The Ca, Al‐rich nodules in the AOAs may be petrogenetically related to the Ca, Al‐rich minerals in Wark‐Lovering rims on type A CAIs. AOAs are chondrite components that condensed during the final stage of Wark‐Lovering rim formation but, in general, were temporally, spatially, or kinetically isolated from reacting with the nebula vapor during condensation of the lower temperature minerals that were commonly present as chondrule precursors.  相似文献   

THE PARENT STRATUM AND DISTRIBUTION OF THE GEORGIA TEKTITES     

Harold Povenmire 《Meteoritics & planetary science》1985,20(4):795-799

Seventy-six field expeditions for Georgia tektites have been made to the vicinity of Dodge County, Georgia in an effort to determine the parent formation and distribution pattern by locating new specimens. About 67 new specimens have been recovered; they represent about 9 percent of all known specimens. The primary area of distribution is a fan shaped area approximately 30 by 72 kilometers. It is likely that these tektites have been transported by water from the parent formation. No correlation could be found between size, shape, soil type, elevation and tektite location. Georgia tektites have previously been found only in strata much younger than their 34 m.y. radiometric age. Here, however, the parent formation is identified as the Tobacco Road Sand of this age.  相似文献   

The petrogenesis of type B1 Ca‐Al‐rich inclusions: The spinel perspective     

Harold C. CONNOLLY  D. S. BURNETT  Kevin D. McKEEGAN 《Meteoritics & planetary science》2003,38(2):197-224

Abstract— Minor element variations in MgAl₂O₄ spinel from the type B1 calcium‐aluminum‐rich inclusion (CAI) Allende TS‐34 confirm earlier studies in showing correlations between the minor element chemistry of spinels with their location within the inclusion and with the chemistry of host silicate phases. These correlations result from a combination of crystallization of a liquid produced by re‐melting event(s) and local re‐equilibration during subsolidus reheating. The correlation of the Ti and V in spinel inclusions with the Ti and V in the adjacent host clinopyroxene can be qualitatively explained by spinel and clinopyroxene crystallization prior to melilite, following a partial melting event. There are, however, difficulties in quantitative modeling of the observed trends, and it is easier to explain the Ti correlation in terms of complete re‐equilibration. The correlation of V in spinel inclusions with that in the adjacent host clinopyroxene also cannot be quantitatively modeled by fractional crystallization of the liquid produced by re‐melting, but it can be explained by partial re‐equilibration. The distinct V and Ti concentrations in spinel inclusions in melilite from the edge regions of the CAI are best explained as being affected by only a minor degree of re‐equilibration. The center melilites and included spinels formed during crystallization of the liquid produced by re‐melting, while the edge melilites and included spinels are primary. The oxygen isotope compositions of TS‐34 spinels are uniformly ¹⁶O‐rich, regardless of the host silicate phase or its location within the inclusion. Similar to other type B1 CAIs, clinopyroxene is ¹⁶O‐rich, but melilite is relatively ¹⁶O‐poor. These data require that the oxygen isotope exchange in TS‐34 melilite occurred subsequent to the last re‐melting event.  相似文献   

Comparison of Station Errors in Seismology     

Harold Jeffreys  Kehar Singh 《Geophysical Journal International》1973,32(4):423-437

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Dynamics of the moon     

Harold Jeffreys 《Physics of the Earth and Planetary Interiors》1971

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First-order and second-order 3-D hydrodynamles: A comparison     

Harold A. Williams 《Celestial Mechanics and Dynamical Astronomy》1988,45(1-3):89-92

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Small Corrections in the Theory of Surface Waves     

Harold Jeffreys 《Geophysical Journal International》1961,6(1):115-117

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The Reduction of Gravity Observations     

Harold Jeffreys 《Geophysical Journal International》1959,2(1):42-44

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Spectral information from fourier analysis of digitized quartz grain profiles     

John D. Boon III  David A. Evans  Harold F. Hennigar 《Mathematical Geology》1982,14(6):589-605

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