Tracing the Electron Density from the Corona to 1 au     

Yolande Leblanc  George A. Dulk  Jean-Louis Bougeret 《Solar physics》1998,183(1):165-180

We derive the electron density distribution in the ecliptic plane, from the corona to 1 AU, using observations from 13.8 MHz to a few kHz by the radio experiment WAVES aboard the spacecraft Wind. We concentrate on type III bursts whose trajectories intersect the spacecraft, as determined by the presence of burst-associated Langmuir waves, or by energetic electrons observed by the 3-D Plasma experiment. For these bursts we are able to determine the mode of emission, fundamental or harmonic, the electron density at 1 AU, the distance of emission regions along the spiral, and the time spent by the beams as they proceed from the low corona to 1 AU. For all of the bursts considered, the emission mode at burst onset was the fundamental; by contrast, in deriving many previous models, harmonic emission was assumed.By measuring the onset time of the burst at each frequency we are able to derive an electron density model all along the trajectory of the burst. Our density model, after normalizing the density at 1 AU to be ne(215 R0)=7.2 cm–3 (the average value at the minimum of solar activity when our measurements were made), is ne=3.3×105 r–2+4.1×106 r–4+8.0×107 r–6 cm–3, with r in units of R0. For other densities at 1 AU our result implies that the coefficients in the equation need to be multiplied by n _e (1 AU)/7.2.We compare this with existing models and those derived from direct, in-situ measurements (normalized to the same density at 1 AU) and find that it agrees very well with in-situ measurements and poorly with radio models based on apparent source positions or assumptions of the emission mode. One implication of our results is that isolated type III bursts do not usually propagate in dense regions of the corona and solar wind, as it is still sometimes assumed.  相似文献   

Precambrian tidal and glacial clastic deposits: implications for Precambrian Earth–Moon dynamics and palaeoclimate     

George E. Williams 《Sedimentary Geology》1998,120(1-4):55-74

Over the past decade the study of Precambrian clastic tidal rhythmites — stacked laminae of sandstone, siltstone and mudstone that display periodic variations in thickness reflecting a strong tidal influence on sedimentation — has provided accurate palaeotidal and palaeorotational data. Palaeotidal records obtained from tidal rhythmites may be systematically abbreviated, however, and derived periods and frequencies can be misleading. The validity of such values, including past length of day, can be assessed by testing for internal self-consistency through application of the laws of celestial mechanics. Such a test supports the estimated length of day of h derived from the late Neoproterozoic (620 Ma) Elatina–Reynella rhythmites in South Australia, and the indicated mean rate of lunar retreat of cm/year since 620 Ma. The validity of estimated lengths of day obtained from other Precambrian tidal rhythmites remain unverified because the data sets contain only one primary value directly determined from the rhythmites. The Elatina–Reynella data militate against significant Earth expansion at least since 620 Ma, and suggest that the free nutation or ‘tipping' of the Earth's fluid core has undergone a resonance with the Earth's annual forced nutation since the Neoproterozoic. Glaciogenic deposits are readily distinguishable from ejecta resulting from impacts with Earth-crossing bodies. Palaeomagnetic data, based on the geocentric axial dipole model for the geomagnetic field, indicate that Neoproterozoic and Palaeoproterozoic glaciation and cold climate near sea level occurred in low palaeolatitudes. This enigmatic finding may imply global glaciation or an increased obliquity of the ecliptic, and is relevant to modelling the effect of ice sheet formation on the Earth's obliquity history by obliquity–oblateness feedback mechanisms. Through multidisciplinary studies, clastic sedimentology and geophysics together can make substantial contributions to understanding Precambrian Earth–Moon dynamics and global palaeoenvironments.  相似文献   

The effect of temperature-dependent exchange coeeficients on poleward heat flux by oceanic gyres     

Quyen Huynh  George Veronis 《Dynamics of Atmospheres and Oceans》1981,6(1):49-66

The gravitational stability of the air overlying the sea surface is determined by the air-sea temperature difference. Air-sea exchange coeeficients have been shown to increase when the air is unstable and decrease when the air is stable. This stability dependence of the wind stress has been approximated by a linear law relating wind stress to air-sea temperature difference and it has been shown that this thermal feedback generates a warm, Gulf-Stream-like jet emerging from the western boundary current eastward into the interior. Here, the thermal correction is applied tot he wind stress and to the air-sea heat exchange coefficient to study the effects on the circulation and on the poleward heat flux. The basic dynamical model is linear, wind-driven and has an anticyclonic gyre in the southern half and an equally intense cyclonic half in the northern half basin. The thermodynamic model uses the vertically averaged, convective-diffusive heat equation. Thermal feedback leads to a compression of the anticyclonic gyre to a narrower lattitude band near the western boundary and to a warm Gulf Stream extending eastward into the interior. The redistribution of the dynamical properties in the anticyclonic gyre resembles that due to inertial processes. In the cyclonic gyre the changes are quite unlike those due to inertial effects. The main quantitative change is the poleward heat flux across the gyre boundary, which can be several times the value obtained without feedback and should be important for climate studies.  相似文献   

Role of barotropic mechanism in the development of a monsoon depression: A MONEX study     

D. Subrahmanyam  M. K. Tandon  L. George  S. K. Mishra 《Pure and Applied Geophysics》1981,119(5):901-912

The role of barotropic processes in the development of a monsoon depression, formed on 5 July 1979 during MONEX observational period, is studied by considering it as a quasi-geostrophic divergent barotropic instability problem of zonal flow of 3 July 1979 at 700 mb level. Numerical solutions are obtained by initial value approach. The preferred wave has a wavelength of 2750 km, an e-folding time of 4.3 days, a period of 6.5 days and an eastward phase speed of 4.9 ms^–1. Structure of preferred wave is found to be in good agreement with the observed horizontal structure of the depression at 700 mb. Poleward momentum transports are found to predominate over equatorward transports.Parts of this paper were presented at the National Symposium on Early Results of MONEX-1979. 9–12 March 1981, in New Delhi, India.  相似文献   

Freshwater reserves of mid-atlantic coast barrier Islands     

Thomas H. Bolyard  George M. Hornberger  Robert Dolan  Bruce P. Hayden 《Environmental Geology》1979,3(1):1-11

A multiple regression model was constructed for the purpose of predicting barrier island hydrology from easily measureable island characteristics. The model was developed using data obtained from 17 sites on the Outer Banks of North Carolina. The accuracy of the model for predicting key hydrologic variables was evaluated by statistical and graphic procedures. In general, agreement between observed and predicted values of the hydrologic variables was very good, suggesting that the quantity of potable water at various island sites can be estimated without resorting to extensive field investigations. The model was then applied to Assateague Island, a barrier island located off the coasts of Maryland and Virginia. Results indicate that the original model developed for the Outer Banks may be applied to other barrier islands but that errors involved may necessitate corrections in detailed studies. Correction for bias in predictions for Assateague was shown to be possible with limited field data from surface resistivity surveys.  相似文献   

A Study of the Reuse of Reused Water     

Edgar D. Smith  Robert M. Sweazy  George A. Whetstone  R. H. Ramsey 《Ground water》1979,17(4):366-374

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Total mercury content in some marine fish from the Indian Ocean     

Tariq W. Kureishy  M. D. George  R. Sen Gupta 《Marine pollution bulletin》1979,10(12):357-360

Total mercury was estimated in liver, gonads and muscle of some of the marine fishes from the Indian Ocean. The highest mercury concentration was observed in the muscle of sharks while the total mercury concentration was practically non-detectable in the liver and gonads. The range of all the values was 0.09–0.21 ppm (wet weight basis) and is quite low to reflect any possible mercury contamination.  相似文献   

Absorption spectra of Cr3+ in Al2O3 under shock compression     

Tsuneaki Goto  Thomas J. Ahrens  George R. Rossman 《Physics and Chemistry of Minerals》1979,4(3):253-263

Unpolarized absorption spectra of single crystals of Cr³⁺ doped Al₂O₃ (synthetic ruby) have measured using a new, time-resolving, dispersive, streak photographic system over the range ～350 to ～700 nm during a series of shock loading experiments. The crystal field absorptions assigned to the transition ⁴ A _2g→⁴ T _2g were observed to shift in a series of experiments from 555±1 nm at atmospheric pressure to 503±5 nm at 46 GPa. In a single experiment at 32 GPa the ⁴ A _2g→⁴ T _1g transition was observed to shift from 405±1 to 386±5 nm. The present data extrapolate downwards in compression toward the 10 GPa data of Stephens and Drickamer (1961) although both crystal field absorption energies increase considerably less with compression than predicted by the simple ionic point charge model. The single datum observed for the Racah parameter B, 588±38 cm^?1 at 32 GPa, is consistant with previous results to 10 GPa and the trend of decreasing B, with compression expected from the divergence of the data from the point charge model due to increasing covalancy.  相似文献   

Comment on “Pacific Pleistocene paleoclimatic stratigraphies: A comparative analysis of results,” by Mark J. Valencia     

George R. Hallberg  Thomas E. Fenton 《Quaternary Research》1979,12(2):290-291

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Core formation in terrestrial planets     

George H. Shaw 《Physics of the Earth and Planetary Interiors》1979,20(1):42-47

Calculations of the radial distribution of the energy released in core formation indicate that the cores of all the terrestrial planets may be expected to receive a disproportionate share of the gravitational energy released. Since the model of the process used in these calculations favors transfer of energy to the mantle, it is likely that other reasonable models of the process will result in even more energy being deposited in the cores of the early planets. The calculations also show that it is necessary for a certain amount of core phase to separate and accumulate, before the energy released by gravitational settling is sufficient to supply the latent heat of fusion of the core phase. The amount of melting required to reach this point varies according to the total mass of the planet, and mass fraction of core, but is not particularly great (<5% for the Earth to ～ 37% for the Moon). In the case of the Moon, this amount of segregation, although large, amounts to a surface layer about 260 km thick, similar to the proposed depth of early wholesale melting. Core separation in terrestrial planets appears to be a self-sustaining process even for fairly small bodies, provided that a small amount of a dense potential core phase is present. Although it seems likely to occur rapidly (within 10⁶–10⁷ years) even for small (Moon-size) bodies, detailed kinetic models will be necessary to specify the time scale.  相似文献