Analysis of processes leading to localized electron enhancements in the outer radiation belt

New information obtained about >500 keV electron intensity enhancements, which have been observed intermittently close to the outer edge of the electron radiation belt, is used in conjunction with an earlier statistical study by Brown and Stone (1972) to investigate processes which could lead to such structures. The enhancements are typically of ～20 sec duration and occur in a very narrow invariant latitude band, maximally 2° wide. The intensity increase relative to the “normal” background level is up to a factor 10, and the “spike” frequency of occurrence is strongly local time dependent, with more spikes observed in the night and dusk-noon sectors than in the noon-dawn sector. The processes investigated quantitatively are distortions of the magnetospheric topology in the equatorial region, wave-particle interactions and the effects of ionospheric currents. It is shown that the various processes which contribute to equatorial field disturbances can explain the observations.     

A nonlinear analysis of the moon's physical libration in longitude

The Euler equations for the forced physical librations of the Moon have already been solved by using a digital computer to perform the semi-literal mathematical manipulations. Very near resonance, the computer solution for the physical libration in longitude is complemented by the solution of the appropriate Duffing equation with a dissipation term. Because of its apparent proximity to a resonant frequency, the term whose argument is 2 - twice the mean angular distance of the Moon's perigee from the ascending node of its orbit - is especially important. Its phase, which soon should be measurable, is related to the Moon's anelasticity. The term's frequency, in units of the sidereal month, increases as the semi-major axis of the Moon's orbit about the Earth increases. Using the Moon's mechanical ellipticity of Koziel and the rate of increase of the semi-major axis of MacDonald, it is estimated that the 2 term will cross the resonant frequency in 130 million years and, if the rate of energy dissipation is sufficiently low, a transient libration will be induced.     

Announcement Internatioal Society for Diatom Research and Nederlands-Vlaamse Kring van Diatomisten

Announcement Internatioal Society for Diatom Research and Nederlands-Vlaamse Kring van Diatomisten     

Comment on the Brans-Dicke-Bianchi type-III vacuum solution

We wish to point out that the Brans-Dicke-Bianchi type-III vacuum solution recently given by Tiwari and Singh (1984) is not new. Moreover, the solution given has no correct Einstein limit, contrary to what is claimed by these authors. The Ellis-MacCallum vacuum solution in the Einstein case can be obtained from the Brans-Dicke solution first given by Lorenz-Petzold (1984a).     

Cenozoic intra-plate magmatism in the Darfur volcanic province: mantle source, phonolite-trachyte genesis and relation to other volcanic provinces in NE Africa

Chemical and Sr, Nd and Pb isotopic compositions of Late Cenozoic to Quaternary small-volume phonolite, trachyte and related mafic rocks from the Darfur volcanic province/NW-Sudan have been investigated. Isotope signatures indicate variable but minor crustal contributions. Some phonolitic and trachytic rocks show the same isotopic composition as their primitive mantle-derived parents, and no crustal contributions are visible in the trace element patterns of these samples. The magmatic evolution of the evolved rocks is dominated by crystal fractionation. The Si-undersaturated strongly alkaline phonolite and the Si-saturated mildly alkaline trachyte can be modelled by fractionation of basanite and basalt, respectively. The suite of basanite–basalt–phonolite–trachyte with characteristic isotope signatures from the Darfur volcanic province fits the compositional features of other Cenozoic intra-plate magmatism scattered in North and Central Africa (e.g., Tibesti, Maghreb, Cameroon line), which evolved on a lithosphere that was reworked or formed during the Neoproterozoic.     

The determination of the derivatives in Brown's lunar theory

The fundamental matrix solutionT for the variational equations of a Hamiltonian system is symplectic. We use this fact to completeT when it is only partially known. We discuss three cases. The last one gives an easy proof for the method invented by Brown in his lunar theory.Paper presented at the 1981 Oberwolfach Conference on Mathematical Methods in Celestial Mechanics.Dedicated to Victor Szebehely.     

Exact spatially self-similar cosmological models of Bianchi type-fV

We investigate the Einstein field equations for tilted spatially self-similar Bianchi type-_fV spacetimes. The solutions represent anisotropic models which can be made consistent with the observed isotropy.     

MODIS Derived Equilibrium Line Altitude Estimates for Purogangri Ice Cap,Tibetan Plateau,and their Relation to Climatic Predictors (2001–2012)

The variation of the equilibrium line altitude can be used as an indicator for glacier mass balance variability. Snow lines at the end of the ablation period are suitable proxies for the annual equilibrium line altitude on glaciers. We investigate snow lines at Purogangri ice cap on the central Plateau in order to study the interannual variability of glacier mass balance. Datasets of the daily Moderate Resolution Imaging Spectroradiometer snow product MOD10A1 were used to infer transient snow line variability during 2001–2012 and to derive regional‐scale, annual equilibrium line altitude. The Moderate Resolution Imaging Spectroradiometer snow albedo embedded within the snow product was compared with high‐resolution Landsat imagery. An albedo threshold was established to differentiate between ice and snow and the 13th percentile of the altitudes of snow‐covered pixels was chosen to represent the snow line altitude. The second maximum of the snow line altitudes in the ablation period was taken as a proxy for the annual equilibrium line altitude. A linear correlation analysis was carried out (1) between interannual variability of the equilibrium line altitude at Purogangri ice cap and various climate elements derived from the High Asia Reanalysis, and (2) between interannual variability of the equilibrium line altitude and the circulation indices North Atlantic Oscillation and Indian Summer Monsoon. Results suggest that air temperature and meridional wind speed above ground in July, as well as the lower tropospheric zonal wind in June and August play a crucial role in the development of the annual equilibrium line altitude.     

The solar system abundances of phosphorus and titanium and the nebular volatility of phosphorus

Abstract— The bulk chemical composition of Orgueil and 25 other carbonaceous chondrites was determined by x‐ray fluorescence analysis. The sample sizes of the analyzed meteorites were in all cases 120 mg. The abundances of P and Ti in Orgueil and Ivuna were precisely determined by the standard addition method. The new P CI abundance is 926 ± 65 ppm. Excluding the low P of Ivuna and one Orgueil sample with unusual chemistry gives a CI P content of 930 ± 23 ppm. A CI abundance of 926 ppm corresponds to a P/Si wt ratio of 8.66 times 10^?3 (atomic ratio 7.85 times 10^?3). For Ti a CI content of 458 ± 18 ppm and a Ti/Si wtratio of 4.28 times 10^?3 (atomic ratio 2.51 times 10^?3) were found. A Si content of 10.69% was obtained for average CI. The new P CI abundance is 20 to 30% below earlier estimates, while the Ti CI abundance is in agreement with earlier determinations. From the results of the analyses of bulk carbonaceous chondrites it is concluded: (1) Refractory element/Mg ratios increase from CI through CM and C3O to C3V, but ratios among Al, Ca and Ti are constant, except for low Ca/Al ratios in the reduced subgroup of C3V. (2) The Si/Mg ratios are constant in all groups of carbonaceous chondrites. (3) There is a volatility related depletion of Cr and Fe, but the Cr/Fe ratios are constant. (4) The sequence of volatility related depletions of the moderately volatile elements P, Au, As, Mn, and Zn follows condensation temperatures (except for As), if in condensation calculations non‐ideal solid solution in the host phase is considered.