Laplace series for the level ellipsoid of revolution

The outer gravitational potential V of the level ellipsoid of revolution T is uniquely determined by two quantities: the eccentricity \(\varepsilon \) of the ellipsoid and Clairaut parameter q, proportional to the angular velocity of rotation squared and inversely proportional to the mean density of the ellipsoid. Quantities \(\varepsilon \) and q are independent, though they lie in a rather strict two-dimensional domain. It follows that Stokes coefficients \(I_n\) of Laplace series representing the outer potential of T are uniquely determined by \(\varepsilon \) and q. In this paper, we have found explicit expressions for Stokes coefficients via \(\varepsilon \) and q, as well as their asymptotics when \(n\rightarrow \infty \). If T does not coincide with a Maclaurin ellipsoid, then \(|I_n|\sim B\varepsilon ^n/n\) with a certain constant B. Let us compare this asymptotics with one of \(I_n\) for ellipsoids constrained by the only condition of increasing (even nonstrict) of oblateness from the centre to the periphery: \(|I_n|\sim \bar{B}\varepsilon ^n/(n^2)\). Hence, level ellipsoids with ellipsoidal equidensites do not exist. The only exception represents Maclaurin ellipsoids. It should be recalled that we confine ourselves by ellipsoids of revolution.     

Registering from Space the Features of Deep Wastewater Outfalls into Coastal Water Areas Due to Discharge Collector Breaks

Izvestiya, Atmospheric and Oceanic Physics - The results of comprehensive studies of anthropogenic impacts caused by deep water discharge into coastal waters near the city of Sevastopol using an...     

Tolman's formula in scalar-tensor theories of gravitation

Erevan State University; Institute of Applied Problems of Physics, Armenian Academy of Sciences. Translated from Astrofizika, Vol. 34, No. 2, pp. 265–270, March–April, 1991.     

Effect of field-aligned currents in the polar cap at the recovery phase of a magnetic storm

Unusually great fluctuations in the ΔB module of the geomagnetic field have been observed in the polar cap from the satellite Cosmos-321. They are explained by small-scale two-sheet field-aligned current systems which exist during the periods when magnetic fields having a considerable northward B_z(B_z 10 nT) component are observed in interplanetary space.     

Moment of inertia of a neutron star. II. Relativistic corrections

In part I we suggested an approximate equation to determine the contribution of relativistic effects to the moment of inertia of a superdense star. In the present paper it is tested on model neutron stars with nine different variants of the equation of state of superdense matter. It is established that the approximation error does not exceed 5% for stable configurations. A more accurate version of the Ravenhall—Pethick equation [D. G. Ravenhall and C. J. Pethick, Astrophys. J., 424, 846 (1994)] for the moment of inertia as a function of the mass and radius of a neutron star is derived. Translated from Astrofizika, Vol. 40, No. 4, pp. 507–516, October–December, 1997.     

Photometric and spectroscopic study of silicon Ap-star HD193722

The period of light variationP=1 _. ^d 13316 has been found for the silicon B9 IVp star HD 193722. Spectroscopic study of this star was based on 35 spectrograms with dispersion 4 Å mm^–1 well distributed in phase. The measurements of radial velocities of spectral line components for SiII, HeI, EuII, FeII and SrII allowed us to localize several regions on the surface of the star with enhanced abundance of these elements. The phase of maximum light inU, B andV was found to be the same as the phase of maximum Eu abundance. The coincidence of the regions with larger abundance of Si and He in HD 193 722 disagree with the hypothesis of diffusion in the presence of a magnetic field developed by Michaud (1971), to explain the peculiar chemical composition of Ap-stars.HD 193722 is a silicon B9 IVp star for which the magnetic field has not been measured. In the list by Palmeret al. (1962) its rotational velocityV sini is given as 250 kms^–1. As will be seen below, this value is too high. Megessier (1971) determined from hydrogen line profiles and continuous spectrumT _eff=13 000° and lgg=3.5.The results of photometric and spectroscopic study of HD193722 are given below.     

贵州铝土矿含矿岩系中锂的分布特征及富集机理

锂是我国关键矿产和高新产业发展的战略性资源之一。贵州铝土矿资源丰富,含铝岩系分布广,勘查发现铝土矿(岩)中伴生大量的锂资源。研究认为,全省含铝岩系中Li含量高,变化范围大(0.55×10^-6～2725.03×10^-6),平面上Li含量总体呈北东(务正道成矿区)、南西(修文-清镇成矿区)高,中间(播州-瓮安成矿区)低的分布态势;剖面上Li主要富集在矿系上部的致密状铝土岩(矿)中,Li含量一般>500×10^-6,矿系中土状铝土矿(岩)Li含量一般<30×10^-6;气候温湿、风化及淋滤作用强的陆相湖泊沉积环境,有利于高岭石为主的黏土矿物形成及Li⁺与Al³⁺、Mg²⁺、Fe³⁺、Fe²⁺发生类质同象,或被吸附进入黏土矿物层间构造同迁移同富集,Li与Al₂O₃含量呈正相关关系;成岩成矿后的次生改造阶段,古地磁测量及CIA显示为炎热潮湿的氧化环境...