Gravity changes accompanying volcanic activity at Pacaya volcano, Guatemala

Gravity changes of up to 1.2 ± 0.1 mgal (1 standard deviation) were measured at three points within 400 m of an active vent on Pacaya volcano, Guatemala during eleven days of January, 1975. For five continuous days gravity varied inversely with the average muzzle velocity of ejecta, the frequency of volcanic explosions, and the frequency of volcanic earthquakes. The gravity changes are most reasonably interpreted as the product of intravolcanic movements of magma with masses one to two orders of magnitude larger than any flow ever erupted from the volcano. However, elevation changes and/or combination of elevation and mass distribution changes could also have been an important factor in effecting the observed gravity variations. Because we lack elevation control on the gravity stations, we are unable to unequivocally conclude which factor or which combination of factors produced the gravity changes. The study indicates the possibility of gravity monitoring of hazardous volcanoes as a predictive tool, and as an added means for investigating the internal mechanism of volcanic eruptions.     

Spectroscopic evidence for aqueous alteration products on the surfaces of low-albedo asteroids

High-resolution IR spectra (0.9–2.5 μm) and narrowband photometry (3.0–3.5 μm) are presented for asteroids 1 Ceres, 2 Pallas and 324 Bamberga. Laboratory experiments with hydrated minerals indicate that the 3 μm absorption feature observed on asteroids is largely due to interlayer water molecules in clay minerals, with a possible contribution from water molecules bound to salts. The depth of the 3 μm band as a function of 2.2 μm albedo is a useful measure of the amount of hydrated mineral present on these asteroids. 1 Ceres must consist mostly of a clay mineral like that in CM chondrites, with some contribution to the strength of the 3 μm band by hydrated salts. These salts, which are products of aqueous alteration, may also be responsible for Ceres' high albedo relative to other C-type asteroids. 2 Pallas must have a low abundance of hydrated minerals relative to 1 Ceres, with the bulk of its composition being spectrally featureless minerals such as the iron-free silicates in CM chondrules. 324 Bamberga probably contains clay minerals, but their abundance cannot be determined at present. The spectrum of Bamberga below 2.5 μm shows evidence for abundant magnetite, which can be a product of aqueous alteration. The presence of magnetite on Bamberga and possibly other C-type asteroids may be responsible for their low albedos. The spectra of C-type asteroids may be reconcilable with those of carbonaceous chondrites if the asteroids surfaces have undergone alteration by aqueous or other analogous processes.     

Spectroscopic evidence for two achondrite parent bodies: asteroids 349 Dembowska and 4 Vesta

A Fourier spectrometer was used to obtain IR spectra of asteroids 349 Dembowska and 4 Vesta (0.8–2.5μm; 25cm ^?1 resolution). The spectrum of Dembowska shows olivine and pyroxene (Fs_{24 ± 8}) with an olivine/pyroxene abundance ratio greater than 2, and possibly as high as 10. This is probably an unsampled achondritic composition, similar to the unique achondrite ALHA 77005. Similar olivine-rich compositions have also been proposed for the mantles of basaltic achondrite parent bodies. Dembowska's mineralogy therefore appears related in some way to the achondrites. but a direct link cannot as yet be made. Our IR observations of Vesta have more complete spectral coverage than those first obtained by Larson and Fink (1975b). Pyroxene (Fs_{50 ± 5}) and plagioclase feldspar are both seen, with a pyroxene/feldspar abundance ratio between 1.5 and 2.0. Vesta's mineralogy is consistent with a mixture of eucrites and howardites on its surface. Time-resolved observations over one-half of the rotation period show no spectral variations at the 2% level, indicating compositional homogeneity. Both 349 Dembowska and 4 Vesta can be considered as candidates for the parent bodies of igneous meteorites.     

Potassium-argon dating of polyhalite in southeastern New Mexico

Polyhalite, K₂Ca₂Mg (SO₄)₄-2H₂O, is an important mineral in many evaporites. Although its use for K-Ar dating has never been investigated, our results indicate that it is a very useful mineral for dating events ranging from the time of potash mineralization to any younger events which may have affected the evaporite. Five K-Ar dates on pure polyhalite, including two from included material and from beds distorted by the formation of a rubble chimney, yield dates between 198 and 216 Myp, in good agreement with Rb-Sr dates and the diagenetic age of the potash deposits from the same rocks. Two polyhalites mixed with sylvite gave lower dates (154 and 174 Myr) which is to be expected because of radiogenic ⁴⁰Ar loss from the sylvite phase. One polyhalite, formed after the intrusion of a 31 Myr lamprophyre dike, yielded 21 Myr. Collectively our results indicate that pure polyhalite is satisfactory for K-Ar dating and may provide critical age information in studies of the geologic history of the evaporite sequences.     

Conditions of generation of a stationary dipole magnetic field

Summary With the aid of the selected spherical model the conditions of generation of a stationary magnetic dipole field in a fluid electrically conducting spherical region, bounded by an outer unconducting region, are derived. It is assumed that there exist turbulent motions in the conducting medium, as well as differential rotation. The induction MHD equation is solved under appropriate boundary conditions. It was found that a stationary dipole field may only be generated at a certain positive value of the coefficient G which characterizes the geometric and physical parameters of the conducting region. If this coefficient is zero, the amplitudes of the magnetic fields decrease exponentially with time.     

Numerical treatment of the kinematic dynamo model

Summary Since the initial equations are complicated, the treatment of the kinematic dynamo model requires the use of numerical methods. In applying them to the given problem difficulties are encountered, which are not easy to overcome. This paper deals with the analysis of the experience acquired in treating the model of a nearly symmetric dynamo. Three different methods were employed (stationary, oscillatory and general non-stationary), because a combination of several solutions will yield more comprehensive information about the model being studied. Although the results are based on the study of a single particular model, similar problems also occur in other excercises and, therefore, the conclusions have a more general validity.     

On the diffusion of the perturbing toroidal magnetic field from the core to the mantle

Zusammenfassung Es werden die Wurzeln einer charakteristischen Gleichung für die Randbedingung der Diffusion des toroidalen magnetischen Störungsfeldes berechnet, das in dünner Schicht unterhalb der Grenze Kern — Mantel, als eine Folge von Störung der Winkelgeschwindigkeit dieser Schicht in Anwesenheit des magnetischen Dipolfeldes induziert wird. Die Wurzeln werden für verschiedene Werte des Verhältnisses der Leitfähigkeit des Erdmantels und Erdkerns ausgerechnet. Es wird gezeigt, dass das aus dem Milieu mit der elektrischen Leitfähigkeit in das Milieu mit elektrischer Leitfähigkeit _m diffundierende toroidale magnetische Störungsfeld vom Werte _m/<10^–2 an von dem Verhältnis elektrischer Leitfähigkeiten beider Milieus unabhänging bleibt.