Isotopes of rubidium in the Sun

Photoelectric measurements of photospheric velocity fields have been carried out with the Sacramento Peak Doppler Zeeman Analyzer. Emphasis was given to long periods and low spatial wavenumbers in deep photospheric layers, where the 5-min oscillations are less dominant.Multiple or double peaks cannot be detected in power spectra of the 5-min oscillations, provided that a sufficient number of physically independent points on the solar surface are observed.The most frequent wave-numbers in the spectra of 5-min oscillations (as well as of the low frequency field) agree with those derived from a model assuming statistically independent oscillators of 10 to 20 diameter. These two velocity fields are anti-correlated spatially.Kinetic power in the 20-to-50-min range of periods is closely linked to brightness changes in the same layer, an increase of brightness lagging about 250 sec behind rising motion. Granules can be excluded as a possible source for the appearance of low frequency flow patterns. Different explanations are suggested.On leave from Fraunhofer Institut, Freiburg, Germany.     

Mass-luminosity ratio in NGC 5236

The mass-to-light ratio in NGC 5236 was studied in terms of four spheroids. The resulting values are quite small and increasing from the centre outwards, suggesting that Population I stars are rather uniformly distributed over its body with a certain concentration towards the central region.     

Pumpellyit (Lotrit) von der Lieserschlucht bei Spittal a. d. Drau,Kärnten

Zusammenfassung Ein lange unbestimmtes, nadeliges Mineral aus der bekannteu, mineralreichen Kalksilikatparagenese von der Lieserschlucht (Lit. 4) wurde optisch und röntgenographisch alsPumpellyit (Lotrit) identifiziert.     

Aufgaben der Felsmechanik bei neuzeitlichen Tunnelrekonstruktionen

Zusammenfassung Aufgaben der Felsmechanik bei neuzeitlichen Tunnelrekonstruktionen. Für die neuzeitliche Tunnelbauweise müssen neue Erkundungsmethoden mit erweitertem Umfang felsmechanischer Prüfungen angewandt werden. Diese Forderung soll ebenso bei Rekonstruktionen erfüllt werden. Außer den mechanischen Eigenschaften werden auch die innere Spannung im Felsmassiv und in der Ausmauerung, die Mächtigkeit der gelockerten Zone sowie die Injektions- und Verankerungsmöglichkeit bestimmt.

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Summary The Function of Rock Mechanics in Modern Tunnelling. For modern methods of tunnel driving it is necessary to apply new procedures of geological investigations including large-scale rock mechanics tests. This view holds equally for reconstruction projects. In addition to the mechanical properties of the rock masses it is necessary to determine the intrinsic stresses in the rock and in the tunnel lining, the thickness of the inelastic (relaxed) zone around the tunnel, as well as the possibility of grouting and anchoring.

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Résumé Application de la mécanique des roches aux méthodes modernes de construction et de reconstruction des tunnels. Dans la technique moderne des tunnels il est nécessaire d'appliquer de nouvelles méthodes de reconnaissance comportant davantage d'essais de mécanique des roches. La même exigence est valable pour la reconstruction des tunnels. Outre les propriétés mécaniques du massif rocheux, on déterminera aussi les contraintes dans le rocher et dans le revêtement, l'épaisseur de la zone décomprimée et même les possibilités d'injection et de boulonnage.

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Vortrag, gehalten beim XIX. Geomechanik-Kolloquium in Salzburg am 17. Oktober 1969.

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Mit 2 Abbildungen     

The precession and nutation of deformable bodies,III

In preceding papers of this series (Kopal, 1968; 1969) the Eulerian equations have been set up which govern the precession and nutation of self-gravitating fluid globes of arbitrary structures in inertial coordinates (space-axes) as well as with respect to the rotating body axes; with due account being taken of the effects arising from equilibrium as well as dynamical tides.In Section 1 of the present paper, the explicit form of these equations is recapitulated for subsequent solations. Section 2 contains then a detailed discussion of the coplanar case (in which the equation of the rotating configuration and the plane of its orbit coincide with the invariable plane of the system); and small fluctuations in the angular velocity of axial rotation arising from the tidal breathing in eccentric binary systems are investigated.In Section 3, we consider the angular velocity of rotation about theZ-axis to be constant, but allow for finite inclination of the equator to the orbital plane. The differential equations governing such a problem are set up exactly in terms of the time-dependent Eulerian angles and , and their coefficients averaged over a cycle. In Section 4, these equations are linearized by the assumption that the inclinations of the equator and the orbit to the invariable plane of the system are small enough for their squares to be negligible; and the equations of motion reduced to their canonical form.The solution of these equations — giving the periods of precession and nutation of rotating components of close binary systems, as well as the rate of nodal regression which is synchronised with precession — are expressed in terms of the physical properties of the respective system and of its constituent components; while the concluding Section 6 contains a discussion of the results, in which the differences between the precession and nutation of rigid and fluid bodies are pointed out.     

Moonquakes and lunar tectonism

With the succesful installation of a geophysical station at Hadley Rille, on July 31, 1971, on the Apollo 15 mission, and the continued operation of stations 12 and 14 approximately 1100 km SW, the Apollo program for the first time achieved a network of seismic stations on the lunar surface. A network of at least three stations is essential for the location of natural events on the Moon. Thus, the establishment of this network was one of the most important milestones in the geophysical exploration of the Moon. The major discoveries that have resulted to date from the analysis of seismic data from this network can be summarized as follows:

1. Lunar seismic signals differ greatly from typical terrestrial seismic signals. It now appears that this can be explained almost entirely by the presence of a thin dry, heterogeneous layer which blankets the Moon to a probable depth of few km with a maximum possible depth of about 20 km. Seismic waves are highly scattered in this zone. Seismic wave propagation within the lunar interior, below the scattering zone, is highly efficient. As a result, it is probable that meteoroid impact signals are being received from the entire lunar surface.
2. The Moon possesses a crust and a mantle, at least in the region of the Apollo 12 and 14 stations. The thickness of the crust is between 55 and 70 km and may consist of two layers. The contrast in elastic properties of the rocks which comprise these major structural units is at least as great as that which exists between the crust and mantle of the earth. (See Toks?zet al., p. 490, for further discussion of seismic evidence of a lunar crust.)
3. Natural lunar events detected by the Apollo seismic network are moonquakes and meteoroid impacts. The average rate of release of seismic energy from moonquakes is far below that of the Earth. Although present data do not permit a completely unambiguous interpretation, the best solution obtainable places the most active moonquake focus at a depth of 800 km; slightly deeper than any known earthquake. These moonquakes occur in monthly cycles; triggered by lunar tides. There are at least 10 zones within which the repeating moonquakes originate.
4. In addition to the repeating moonquakes, moonquake ‘swarms’ have been discovered. During periods of swarm activity, events may occur as frequently as one event every two hours over intervals lasting several days. The source of these swarms is unknown at present. The occurrence of moonquake swarms also appears to be related to lunar tides; although, it is too soon to be certain of this point.

These findings have been discussed in eight previous papers (Lathamet al., 1969, 1970, 1971) The instrument has been described by Lathamet al. (1969) and Sutton and Latham (1964). The locations of the seismic stations are shown in Figure 1.     

Dynamical tides in close binary systems

The aim of the present paper will be to deduce the explicit form of differential equations which govern dynamical tides in close binary systems, with simplifications which are permissible for the mass-point model (Section 2), as well as for one exhibiting finite but high internal density concentration (Section 3). It is pointed out that, whereas the exact formulation of the problem leads to a simultaneous system of equations of sixth order (fourth in the inviscid case), this order reduces to four (or two for inviscid fluids) for the mass-point model; and to five (three for inviscid case) if the density concentration is high but finite.In the last section of this paper the coefficientsC _i,j which specify the amplitudes of the individual partial tides are explicitly formulated as functions of the time.