Das elliptische eingeschränkte Dreikörperproblem

Inhalt Eine einfache Herleitung der allgemeinen Gleichungen des elliptischen eingeschränkten Dreikörperproblems und der daraus folgenden linearen Variationsgleichungen mit periodischen Koeffizienten für die Bewegung in der Nähe der Librationszentren wird gegeben. Die in zwei früheren Arbeiten vorgelegte Aufspaltung der ebenen Variationsgleichungen 4. Ordnung in zwei Komponenten 2. Ordnung wird kurz rekapituliert.Bei Benützung dieser Aufspaltung wird die Bewegung in der Umgebung der Dreieckspunkte näher untersucht. Mit Hilfe einer Näherungslösung werden Frequenzverteilung und Stabilitätsbereiche bestimmt.

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A simple derivation of the general equations of the elliptic restricted Three-Body Problem is given from which immediately follow the linear variational equations with periodic coefficients describing the motion close to the libration centers. The explicit separation of these 4th order planar variational equations into two 2nd order components is shortly repeated.Using this separation the motion in the neighborhood of the equilateral points is investigated in more detail. An approximate solution is determined giving frequency distribution and stability domains.

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Gehalten vor der Konferenz über Celestial Mechanics, Oberwolfach, Germany, August 27–September 2, 1972.     

Interference in solar oscillations

We have analyzed magnetograph observations of the 5-min oscillations. We find that most of the oscillatory power is concentrated in space and frequency. Interference effects where these concentrations overlap can explain some of the variations in amplitude of the oscillation.Of the National Bureau of Standards and University of Colorado.     

Photometric and spectrophotometric observations of Nova Delphini 1967

Photographic, photovisual and photoelectric (V) observations of Nova Delphini 1967 were made from August 8 to October 31 (Table I, Figure 1). Simultaneously spectrophotometric measurements of the continuum were made on objective prism exposures extending to November 26, and spectrophotometric gradients derived (Tables II and III; Figures 3, 4, and 5). The continuum of Nova near its flat maximum is close to that of an early-type star in contrast to late-type absorptionline spectrum.     

High-resolution measurements of photosphere and sunspot velocity and magnetic fields using a narrow-band birefringent filter

Modifications to a Zeiss 1/4 Å filter are described which allow high spatial resolution observations of the line-of-sight velocities and magnetic fields in the photosphere and in sunspots. First results show: (1) the granular velocity field to be very strong; differences in upward motions in the granules and downward motions in between are as much as 6 km/sec; (2) the Evershed effect in sunspots to originate primarily in the dark regions between bright penumbral filaments.     

The scattering mean free path in the Uranian atmosphere

New measurements of the equivalent widths of the 4-0 S(0) and S(1) H₂ quadrupole lines in the Uranian spectrum have been obtained using high dispersion (4.12 Å/mm) image-tube spectrography. The measured equivalent widths are $\text{62 ± 19}\text{m}\text{A}\text{?}\text{and}\text{58 ± 13}\text{m}\text{A}\text{?}$ for the S(0) and S(1) lines, respectively. Curve-of-growth analysis in terms of a reflecting layer model yields an H₂ column-density of 780_?330⁺⁹⁴⁰km amagat and a temperature of 78_?24⁺⁸⁰°K. Interpretation using a semi-infinite, homogeneous, isotropically scattering model for line formation yields a scattering mean free path at λ6400 Å of 550 ± 250 km amagat. Quoted errors for both the H₂ column-density and the scattering mean free path include the effect of uncertainty in the choice of atmospheric temperature. The results are discussed in terms of current models for the Uranian atmosphere.     

Theoretical ion densities in the lower ionosphere

We have solved the coupled momentum and continuity equations for NO⁺, O₂⁺, and O⁺ions in the E- and F-regions of the ionosphere. This theoretical model has enabled us to examine the relative importance of various processes that affect molecular ion densities. We find that transport processes are not important during the day; the molecular ions are in chemical equilibrium at all altitudes. At night, however, both diffusion and vertical drifts induced by winds or electric fields are important in determining molecular ion densities below about 200 km. Molecular ion densities are insensitive to the O⁺ density distribution and so are little affected by decay of the nocturnal F-region or by processes, such as a protonospheric flux, that retard this decay. The O⁺ density profile, on the other hand, is insensitive to molecular ion densities, although the O⁺ diffusion equation is formally coupled to molecular ion densities by the polarization electrostatic field. Nitric oxide plays an important role in determining the NO⁺ to O₂⁺ ratio in the E-region, particularly at night. Nocturnal sources of ionization are required to maintain the E-region through the night. Vertical velocities induced by expansion and contraction of the neutral atmosphere are too small to affect ion densities at any altitude.     

On the galactic plane discontinuity nearl=140°

Star counts, from measurements made by the GALAXY measuring machine, in unit B magnitude intervals were made in nine regions, each of 1.75 square degrees distributed about (l, b)= (140°, 0°). The mean density function and the mean variation of interstellar absorption with distance for the various areas were determined using a combination of theoretical and observed cumulative Wolf diagrams. For the same regions multi-colour (UBV) photographic photometry was used to identify early type stars. The distribution of these stars shows three main peaks which correspond well in distance with the Perseus, - and -spiral arms found by Verschuur from radio measurements of neutral hydrogen. The pattern made by the stellar arms in the (l, r) plane shows a discontinuity nearl=140°. From a consideration of both the star counts and the distribution of the reddened early type stars it is suggested that the cause of the discontinuity is a cloud with 0 _. ^m 7 total obscuration situated much nearer to the Sun than the Perseus arm and terminating on one side atl=140°.     

‘Copernicus’ observations of extragalactic X-ray sources

The MSSL X-ray detectors onCopernicus have been used to study a number of extragalactic objects. At least three classes of unresolved sources are found and we suggest that accretion may be the dominant mechanism. The mass of the accreting object then determines the X-ray emission properties.Paper presented at the COSPAR Symposium on Fast Transients in X- and Gamma-Rays, held at Varna, Bulgaria, 29–31 May, 1975.