The ortho- to para- ratio of H₂ in the starburst of NGC 253     

Andrew Harrison  Phil Puxley  Adrian Russell  & Peter Brand 《Monthly notices of the Royal Astronomical Society》1998,297(2):624-632

We present measurements of several near-infrared emission lines from the nearby galaxy NGC 253. We have been able to measure four H₂ lines across the circumnuclear starburst, from which we estimate the ortho- to para- ratio of excited H₂ to be ∼2. This indicates that the bulk of the H₂ emission arises from photodissociation regions (PDRs), rather than from shocks. This is the case across the entire region of active star formation.
As the H₂ emission arises from PDRs, it is likely that the ratio of H₂ to Brγ (the bright hydrogen recombination line) is a measure of the relative geometry of O and B stars and PDRs. Towards the nucleus of NGC 253 the geometry is deduced to be tightly clustered O and B stars in a few giant H  II regions that are encompassed by PDRs. Away from the nuclear region, the geometry becomes that of PDRs bathed in a relatively diffuse ultraviolet radiation field.
The rotation curves of 1–0 S(1) and Brγ suggest that the ionized gas is tracing a kinetic system different from that of the molecular gas in NGC 253, particularly away from the nucleus.  相似文献   

A once-molten,coarse-grained,Ca-rich inclusion in Allende     

Glenn J. MacPherson  Lawrence Grossman 《Earth and Planetary Science Letters》1981,52(1):16-24

A compact, spheroidal Type B inclusion in Allende contains melilite laths that project radially inward from the inclusion edge which show interference growth textures. The combined textural and chemical features of this object cannot be explained by independent vapor-solid condensation of grains in space, followed by random aggregation of these grains into an inclusion. Rather, it probably formed from a once-molten droplet that crystallized in response to radiative cooling from its outer surface. The crystallization sequence in this and another similar inclusion in which oxygen isotopes have been measured is: melilite-spinel-anorthite-fassaite. This sequence supports the idea that oxygen isotopic heterogeneities in coarse-grained inclusions were formed after complete solidification of these objects by partial exchange with a less¹⁶O-rich gas, and not during or before a melting event.  相似文献   

Ca isotope fractionation on the Earth and other solar system materials   总被引：1，自引：0，他引：1  

W.A. Russell  D.A. Papanastassiou  T.A. Tombrello 《Geochimica et cosmochimica acta》1978,42(8):1075-1090

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Origin of reverse-graded bedding in air-fall pumice, Coso Range, California     

Wendell A. Duffield  Charles R. Bacon  Glenn R. Roquemore 《Journal of Volcanology and Geothermal Research》1979,5(1-2)

The origin of reverse grading in air-fall pyroclastic deposits has been ascribed to: (1) changing conditions at an erupting vent; (2) deposition in water; or (3) rolling of large clasts over smaller clasts on the surface of a steep slope. Structural features in a deposit of air-fall pumice lapilli in the Coso Range, California, indicate that reverse grading there formed by a fourth mechanism during flow of pumice. Reverse-graded beds in this deposit occur where pumice lapilli fell on slopes at or near the angle of repose and formed as parts of the blanket of accumulating pumice became unstable and flowed downslope. The process of size sorting during such flow is probably analogous to that which sorts sand grains in a reverse fashion during avalanching on the slip faces of sand dunes, attributed by Bagnold (1954a) to a grain-dispersive pressure acting on particles subjected to a shear stress. In view of the several ways in which air-fall pyroclastic debris may become reverse graded, caution is advised in interpretation of the origin of this structure both in modern and in ancient deposits.  相似文献   

The Martian magnetic field     

C.T. Russell 《Physics of the Earth and Planetary Interiors》1979,20(2-4):237-246

The magnetic field measurements of the Mars 2, 3 and 5 spacecraft have been interpreted by Dolginov and co-workers to be consistent with an intrinsic planetary magnetic moment of 2.5 × 10²² gauss cm³. They base this interpretation mainly on the apparent size of the obstacle responsible for deflecting the solar wind, the lack of dependence of the sign of the magnetic field in the wake region of the planet on the sign of the component of the interplanetary field radially out from the sun, and an apparent encounter of the Mars spacecraft with the planetary field. When examined in detail this evidence is very suspect. A detailed criticism of the arguments by Dolginov and co-workers for an intrinsic field has appeared elsewhere. Herein we summarize this criticism and present, in an appendix, a compendium of the Mars 3 and 5 magnetic field data transformed into a coordinate system in which the details of the interaction are more easily visualized. Many of these data have not been published in this form previously.  相似文献   

The radioracemization of isovaline. Cosmochemical implications     

William A. Bonner  Neal E. Blair  Richard M. Lemmon  Jose J. Flores  Glenn E. Pollock 《Geochimica et cosmochimica acta》1979,43(11):1841-1846

The optically pure d- and l-enantiomers of isovaline (I), which cannot be racemized by ordinary chemical mechanisms involving α-hydrogen removal, and which has been isolated in apparently racemic form from the Murchison meteorite, have been subjected to partial radiolysis by the ionizing radiation from a 3000 Ci ⁶⁰Co γ-ray source. Both in the anhydrous and hydrated solid states and as solid sodium or hydrochloride salts each enantiomer suffered significant radioracemization of the undestroyed residue during its partial radiolysis. The sodium salt of isovaline in 0.1 M aqueous solution suffered extensive radiolysis with relatively small radiation doses, but showed no detectable radioracemization. The significance of these observations with respect to the primordial enantiomeric composition of the isovaline (and other amino acids) indigenous to meteroties is discussed.  相似文献   

Seismological services of the Australian Bureau of Mineral Resources,Geology and Geophysics     

P.M. McGregor 《Physics of the Earth and Planetary Interiors》1979,18(2):105-113

The Bureau of Mineral Resources, Geology and Geophysics provides seismological services which complement those provided by several other agencies.The services comprise the operation of 20 seismograph stations in continental Australia, and the operation of regional data centres for earthquakes and strong earth-motion data. The ambit of the data centres includes BMR stations in Antarctica and Papua New Guinea, and foreign stations in Papua New Guinea and the Solomon Islands. Most of the data are lodged at World Data Centres, and the remainder are available from the BMR national centre.The combined Australian network has provided data at a regional level only for about the last twenty years. These have however, been sufficient to show that although seismicity is low it is not insignificant, and that there are several areas where damaging earthquakes can be expected to recur at 50-year intervals; about 500 Australian earthquakes are located annually.Complete national location capability does not extend below Richter magnitude 4, and it is unlikely that significant improvements can be expected in the near future. In most of the areas where earthquake risk is important from a civil standpoint the detection capability is about magnitude 3. For the other more remote areas advanced techniques based on unattended seismometers and satellite telemetry will probably be needed to attain the same capability.  相似文献   

Radiance and color of the sky at twilight: Perturbations caused by stratospheric haze     

Glenn E. Shaw 《Pure and Applied Geophysics》1980,119(2):231-247

Layers of stratospheric aerosol with optical thicknesses as small as 10^–4 cause noticeable perturbations in the monochromatic logarithmic brightness gradient,G, and the color ratio,C, of the twilight sky. Modeling of the twilight's radiant properties shows that definite single-valued relationships exist between maxima inC or minima inG and optical thickness, , physical thickness h, and mean altitude, , of stratospheric layers. It is therefore possible to determine , h and and monitor their variations by performing either single wavelength measurements ofG or two-wavelength spectrophotometric measurements ofC. The presence of haze in the lower troposphere and the occurrence of multiple scattering both have relatively minor influences on the recovery of the stratospheric dust properties, provided that 10< <30 km.Formal mathematical inversions of the single-scattering twilight equations are possible in principle, but difficult in practice because of non-linearities. Inversions incorporating an iterative linearization process with constrained smoothing, successfully recovered the features of the haze layer, but tended to oversmooth the vertical profile and underestimate the mean altitude of the haze layer.  相似文献   

Electron microprobe study of a ‘mysterite’-bearing inclusion from the Krymka LL-chondrite     

Lawrence Grossman  John M. Allen  Glenn J. MacPherson 《Geochimica et cosmochimica acta》1980,44(2):211-216

The black inclusion from the Krymka LL3 chondrite previously found to contain ‘mysterite’ by Lewiset al. (1979) belongs to a hitherto unknown class of carbonaceous chondrites. Its olivine and pyroxene compositions. Fo 97–99 and En 96, respectively, are characteristic of carbonaceous chondrites and its plagioclase composition. An 100, is characteristic of C3's. It contains a peculiar group of Co-, Cr-rich metal grains whose compositions are similar, but not identical, to those in C2 chondrites and which also bear some similarities to those in Renazzo. Its weight ratios of total $\text{Fe}\text{SiO}{}_2$ and $\text{solSiO}{}_2\text{MgO}$ are 0.74 and 1.43, respectively, and its atomic ratio of $\text{Si}\text{Al}$ is 10.7, exactly the same as in carbonaceous chondrites. Its bulk chemical composition is very close to that of the Murchison C2 chondrite. The association of mysterite with a special type of carbonaceous chondrite material suggests that mysterite formed by low-temperature condensation in a different region of the nebula from other carbonaceous chondrites.  相似文献   

Observations on the asexual reproductive activities of the sessile stages of the sea nettleChrysaora quinquecirrha (Scyphozoa)     

David G. Cargo  Glenn E. Rabenold 《Estuaries and Coasts》1980,3(1):20-27

Twenty-seven colonies of wild scyphistomae ofChrysaora quinquecirrha were observed for a period of ten weeks during the summer. Asexual activities of individual organisms were recorded several times each week. Polyps most often proceeded to strobilate in mid-June and then strobilate a second time 18 days later. They then detached and changed position by means of stolons and then produced podocysts. Initial cysts first excysted and the resulting polyps then strobilated. A second strobilation was not generally observed. The developmental implications of these activities are discussed.  相似文献