On the nature of the anti-tail of Comet Kohoutek (1973f). II. Comparison of the working model with ground-based photographic observations

Photographic observations of the anti-tail of Comet Kohoutek (1973f), obtained at the Cerro Tololo Inter-American Observatory, are photometrically reduced and the results compared with a recently formulated working model of the anti-tail. The applied technique of photometric reduction is described, and the radial and transverse profiles of the anti-tail, corrected for the effects of atmospheric extinction and the variable intensity of the ambient sky, are derived. Brightness variations in time are also studied. The most important result reached so far is a quantitative confirmation of the previously suggested hypothesis, arguing that dust particles in the anti-tail suffered a significant loss in radius due to evaporation near the perihelion passage. We find that only particles initially larger than 100–150 μm in diameter (at an assumed density of 1 gcm^?3) survived. Numerically, however, this result is still preliminary, because the dynamical effect associated with particle evaporation remains to be explained. It is also tentatively suggested that the emission rate of the dust from the comet was probably comparable with the rates derived earlier for Comets Arend-Roland (1957 III) and Bennett (1970 II).     

Mineralogy of metallic phases in sulphide mattes from primary lead smelting

The mattes resulting from lead smelting have been studied in order to determine the distribution of heavy metals and metalloids in primary phases. The chemical analysis (EPMA) revealed the presence of various metals (Pb, Sb, Cu), sulphides (galena, wurtzite, pyrrhotite, bornite, digenite, cubanite), arsenides (koutekite, löllingite) and other complex intermetallic compounds. Extreme saturation of the initial matte melt in heavy metals and metalloids as well as a relatively rapid cooling regime are responsible for numerous elemental substitutions in the crystal structures of all the involved phases. To cite this article: V. Ettler, Z. Johan, C. R. Geoscience 335 (2003).     

Natural alteration products of sulphide mattes from primary lead smelting

The natural alteration products developed on mattes from lead metallurgy were determined: oxides and hydroxides (HFO, Cu(OH)₂), sulphates (thenardite, gypsum), hydroxysulphates (jarosite, beaverite, brochantite) and carbonates (cerussite, malachite, NaOH·2 PbCO₃). The large range of stability of newly formed phases confirms a significant variety of E_h–pH conditions of natural weathering of matte. Jarosite is stable at pH<3, but some hydroxides and carbonates typically form in neutral and alkaline environments. Consequently, the best dumping conditions for metallurgical mattes are difficult to determine. Such materials can have severe environmental effects and should be dumped in controlled waste-disposal sites. To cite this article: V. Ettler et al., C. R. Geoscience 335 (2003).     

Relative motions of fragments of the split comets.: I. A new approach

A new approach is formulated for the study of motions of the split comets. It is based on the assumption that two fragments of a comet separate at a rate that is determined primarily by a slight difference between their effective solar attractions rather than by the impulse imparted on them at the time of splitting. The net dynamical effect is interpreted as due to differential nongravitational forces, which depend on the size, density, structure, composition, and spin rate of the fragments. Since at least at smaller distances from the Sun these forces vary inversely as roughly the square of heliocentric distance, their dynamical effect resembles that of radiation pressure, so that the formalism developed for the motion of a dust particle in a cometary tail is applicable in principle. The calculations show that this approach provides reasonably good to excellent fits of the observed separations for a great majority of the split comets, and that it fails only in the case of Comet 1957 VI. The correlation between the differential nongravitational forces and the endurance of the fragment is investigated in terms of the physical behavior of the fragments, with the emphasis on the short-lived objects. Some of the unusual phenomena accompanying the split comets are discussed, and comments are also offered on the sequence of splitting for comets with multiple nuclei and on the distribution of the points of splitting in space.     

Relative motions of fragments of the split comets: II. Separation velocities and differential decelerations for extensively observed comets

A multiparameter model has been devised to discriminate the effects of the velocity of separation of two fragments of a split comet on their observed motions from the effects of the postsplit differential nongravitational forces. The iterative differential-correction procedure is applied to five extensively observed split comets: West 1975n, Ikeya-Seki 1965 VIII, Wirtanen 1957 VI, the Southern Comet 1947 XII, and Periodic Brooks 2 1889 V. The present model confirms that the major contribution to the observed rate of separation of the fragments comes from the postsplit forces. The model removes or substantially reduces the systematic trends in the residuals of comets West, Wirtanen, and P/Brooks 2, which could not be eliminated by a simple model that ignored the effects of the separation velocity. In particular, the results for Comet Wirtanen now indicate that the comet split at a heliocentric distance of more than 9 AU and that the initial rate of separation of the two fragments did not amount to more than 26 cm/sec. The separation velocities for the other comets range from 1 to 2 m/sec. Difficulties of the interpretation of the observed separation velocities are briefly discussed.     

Properties of altered coals associated with Carboniferous red beds in the Upper Silesian Coal Basin and their tentative classification

In the Czech and Polish parts of the Upper Silesian Coal Basin, red beds associated with the pre-Neoide tectonic structures are found. The occurrence of these beds is connected with changes in the development of the coal seams, in the macroscopic and microscopic character of coal and with its chemical and technological properties. These changes are due to the thermal and oxidation alteration of coal as a result of geological processes which, up to now, have not been clarified unambiguously. These altered coals were divided into groups according to their chemical and physical properties and vitrinite reflectance using statistical multicomponent methods. Coal samples classified as belonging to one of these groups correspond to a certain type of coal, characterized by a particular grade of thermal and oxidation alteration and petrographical composition.     

A probability of encounter with interstellar comets and the likelihood of their existence

A theory of the probability of encounter of the Sun with an interstellar comet at a distance comparable to the Earth-Sun distance is formulated, and a general expression is derived establishing the relationship among the influx rate of interstellar comets, the perihelion distance, the space density of the comets, the Maxwellian distribution of comet velocities in the interstellar cloud, and the cloud's systematic velocity relative to the Sun. The fact that no comet with a strongly hyperbolic orbit has so far been observed is used to determine an upper limit of 6 × 10^?4 solar masses per cubic parsec (4 × 10^?26 gcm^?3) for the space density of interstellar comets. The theoretical distribution of semimajor axes of interstellar comets is derived to show that a strong hyperbolic excess must be present in the orbits of a majority of interstellar comets regardless of the dynamical characteristics of the comet cloud, except when the cloud is moving along with the Sun and the distribution of individual velocities has a very low dispersion. This case, however, implies a possibility of capture by the Sun and thus becomes a problem of an Oort-type cloud.     

Relationships among flare images at different wavelengths

The talk reviews briefly historical development of the imaging of the Sun, and flare imaging in particular, at different wavelengths. The present state is then critically analyzed, emphasizing and demonstrating problems related to simultaneity of observed data, differences in time resolution, limitations of the imaged field of view, unequal spatial resolution, and alignment of the images. Prospects for the future are briefly sketched, including imaging in very hard X-rays and -rays.