The retrieval of cloud microphysical properties using satellite measurements and an in situ database

By combining AVHRR data from the NOAA satellites with information from a database of in situ measurements, large-scale maps can be generated of the microphysical parameters most immediately significant for the modelling of global circulation and climate. From the satellite data, the clouds can be classified into cumuliform, stratiform and cirrus classes and then into further sub-classes by cloud top temperature. At the same time a database of in situ measurements made by research aircraft is classified into the same sub-classes and a statistical analysis is used to derive relationships between the sub-classes and the cloud microphysical properties. These two analyses are then linked to give estimates of the microphysical properties of the satellite observed clouds. Examples are given of the application of this technique to derive maps of the probability of occurrence of precipitating clouds and of precipitating water content derived from a case study within the International Cirrus Experiment (ICE) held in 1989 over the North Sea.     

Geologisch-petrographische Beobachtungen in den Schottischen Highlands

Zusammenfassung In Ergänzung zum FortschrittsberichtKürstens werden geologische Probleme des Schottischen Kristallins diskutiert unter Betonung der petrographischen Betrachtungsweise und Verwertung eigener Feld- und Schliffbeobachtungen.     

Equilibrium coexistence of three amphiboles

Electron probe and wet chemical analyses of amphibole pairs from the sillimanite zone of central Massachusetts and adjacent New Hampshire indicated that for a particular metamorphic grade there should be a restricted composition range in which three amphiboles can coexist stably. An unequivocal example of such an equilibrium three amphibole rock has been found in the sillimanite-orthoclase zone. It contains a colorless primitive clinoamphibole, space group P2₁/m, optically and chemically like cummingtonite with blue-green hornblende exsolution lamellae on (100) and (¯101) of the host; blue-green hornblende, space group C2/m, with primitive cummingtonite exsolution lamellae on (100) and (¯101) of the host; and pale pinkish tan anthophyllite, space group Pnma, that is free of visible exsolution lamellae but is a submicroscopic intergrowth of two orthorhombic amphiboles. Mutual contacts and coarse, oriented intergrowths of two and three host amphiboles indicate the three grew as an equilibrium assemblage prior to exsolution. Electron probe analyses at mutual three-amphibole contacts showed little variation in the composition of each amphibole. Analyses believed to represent most closely the primary amphibole compositions gave atomic proportions on the basis of 23 oxygens per formula unit as follows: for primitive cummingtonite (Na_0.02Ca_0.21 ^– Mn_0.06Fe²⁺ _2.28Mg_4.12Al_0.28) (Al_0.17Si_7.83), for hornblende (Na_0.35Ca_1.56Mn_0.02Fe_1.71Mg_2.85Al_0.92) (Al_1.37Si_6.63), and for anthophyllite (Na_0.10Ca_0.06Mn_0.06Fe_2.25Mg_4.11Al_0.47) (Al_0.47Si_7.53). The reflections violating C-symmetry, on X-ray single crystal photographs of the primitive cummingtonite, are weak and diffuse, and suggest a partial inversion from a C-centered to a primitive clinoamphibole. Single crystal photographs of the anthophyllite show split reflections indicating it is an intergrowth of about 80% anthophyllite and about 20% gedrite which differ in their b crystallographic dimensions. Split reflections are characteristic of all analyzed orthorhombic amphiboles so far examined from Massachusetts and New Hampshire except the most aluminous gedrites, and the relative intensity of the gedrite reflections is roughly proportional to the degree of Na and Al substitution. Thin sections of a few of these anthophyllite specimens show lamellae parallel to (010) that are just resolved with a high power objective.Publication approved by the Director, U.S. Geological Survey.     

Zum Vorkommen von Pyrophyllit,Gümbelit und Quarziten in der Kontaktaureole des Bramscher Massivs

Zusammenfassung Die geophysikalischen Untersuchungen am Störkörper von Bramsche, ca. 20 km N Osnabrück, deuten auf einen basischen Intrusivkörper in ca. 5 km Tiefe. Hohe Inkohlungsgrade in karbonischen bis kretazischen Sedimenten lassen eine starke Wärmequelle mit einem bis zu den Karbonhorsten südlich und westlich Osnabrück reichenden Kontakthof vermuten, mit einem Maximum der Inkohlung im Gebiet der geophysikalischen Anomalie.Während sich an den Karbonhorsten um Osnabrück sulfidisch-barytische Erze kretazischen Alters finden, fehlen jegliche Vererzungsspuren im Zentrum der Anomalie. Hier könnten lediglich Pyrophyllit und Quarzitisierungen im Malm des Gehns und das Vorkommen von Gümbelit im Piesberg-Karbon auf Auswirkungen der Intrusion hinweisen. Ausbildung (Faseraggregate der Phyllosilikate) und geologisches Auftreten (keine laterale Verteilung) sprechen aber für eine im weitesten Sinne lateral-sekretionäre Entstehung.Experimente vonNoll (1936) undAlthaus (1966) ergaben eine Bildungstemperatur für Pyrophyllit von ca. 390° C. Es finden sich jedoch keine pegmatitisch-pneumatolytischen oder katahydrothermalen Mobilisate in diesem Gebiet. Somit sollte die Bildungstemperatur für den Pyrophyllit niedriger gewesen sein. Selbst wenn die Bildungstemperatur bekannt wäre, wäre es schwierig, den hydrothermal gebildeten Pyrophyllit als geologisches Thermometer zu benutzen.- Geothermische Überlegungen zur Kalkulation der Intrusionstemperatur lassen sich hier somit nur noch mit Hilfe des Inkohlungsgrades vornehmen.

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Geophysical researches at the Bramsche anomaly, about 20 km north of Osnabrück in NW-Germany indicate a basic intrusive body at the depth of about 5 km. A big source of heat with a contact zone reaching to the Carboniferous horsts south and west of Osnabrück is supposed by the increase of coalification in Carboniferous up to Cretaceous sediments, which has the highest degrees of coalification in the region of the geophysical anomaly.While there are sulfide deposits with barytic gangue of Cretaceous age at the Carboniferous horsts near Osnabrück, there are no ore-traces in the centre of the anomaly. Only the occurence of pyrophyllite and quartzites in the Malm of the Gehn-hills and the occurrence of gümbelite (Mg-hydromuscovite) in the Carboniferous sediments of Piesberg-horst may indicate the influence of the intrusion. - But habit (fibre-aggregates of the phyllosilicates) and geologic occurence (no lateral distribution) of these mineralisations suggest a formation by lateral secretion in a broader meaning of the term.Experiments byNoll (1936) andAlthaus (1966) proved a temperature of about 390° C for the formation of pyrophyllite. But there are no pegmatitic-pneumatolytic or kata-hydrothermal mobilisations in this district. Therefore it is assumed that the temperature of the formation may be lower under other conditions. Even if the temperature of this formation were known, it would be difficult to use pyrophyllite — formed under hydrothermal conditions — as a geologic thermometer. - Geothermal conclusions to calculate the temperature of the intrusion are only possible by using the decrease of volatile matter of the coals.

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Résumé Les recherches géophysicales du corps failleux de Bramsche, à environ 20 km au nord d'Osnabrück font penser à un corps intrusit basique à 5 km sous la surface. De grands degrés d'houillification en des sédiments carbonifères et crétacés révèlent une forte source de chaleur avec une auréole de contact s'étendant jusqu'aux horsts carbonifères au sud et à l'ouest d'Osnabrück, avec un maximum d'houillification dans la région de l'anomalie géophysicale.Bien qu'on trouve des airains crétacés sulfurés avec barytine, aucune trace de minéralisation n'est visible au centre de l'anomalie. Ce n'est que la pyrophyllite et les quartzites dans le Malm du Gehn et l'existence de gümbelite (Mghydro-muscovite) dans le Piesberg-Karbon qui peuvent indiquer des effets d'intrusion. La structure et l'existence géologique font plutôt penser à une genèse latéralement sécrétionaire. Des conclusions géothermiques pour calculer la température d'intrusion ne sont à entreprendre qu'à l'aide du degré d'houillification.

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Meinem verehrten Lehrer, Herrn Prof. Dr. H.Harder danke ich für die Anregung zu dieser Arbeit im Rahmen einer regionalen lagerstättenkundlichen Dissertation. Für weitere Hinweise und Diskussionen bin ich Herrn Prof. Dr. B.Brockamp verpflichtet.     

Petrology of a ferruginous hornfels from Riekensglück,Harz Mountains,Germany

The hornfels first described by Ramdohr (1927) contains the rare, if not unique, mineral assemblage olivine-cordierite-spinel-garnet-gedrite-biotite(-tourmaline)-FeTi oxides. Mieroprobe analyses of the constituting phases show that their Fe/(Fe+Mg)-ratios increase in the order (tourmaline-) cordierite-biotite-gedrite-olivine-garnet-hercynite-rich spinel. On the basis of the experimental results of Hsu and Burnham (1969) in the system Fe-O-MgO-Al₂O₃-SiO₂-H₂O the metamorphic history of the hornfels is subdivided into an earlier high-temperature stage 1 characterized mainly by the assemblage olivine-cordierite-spinel, and a subsequent, lower-temperature stage 2, in which the additional phases garnet and gedrite grew as porphyroblasts and equilibrated with the other phases. At an estimated mean confining pressure of 500 bars for both hornfels stages the temperatures during stage 1 may have ranged from 600° to about 800° C, whereas during stage 2 only some 550–580° C were attained. It is possible that these two metamorphic stages are due to the consecutive intrusions, first of the gabbroic and then of the granitic magmas.     

On the origin of solar metric type II bursts

The vast majority of solar flares are not associated with metric Type II radio bursts. For example, for the period February 1980–July 1982, corresponding to the first two and one-half years of the Solar Maximum Mission, 95% of the 2500 flares with peak >25 keV count rates >100 c s^–1lacked associated Type II emission. Even the 360 largest flares, i.e., those having >25 keV peak count rates >1000 c s^–1, had a Type II association rate of only 24%. The lack of a close correlation between flare size and Type II occurrence implies the need for a 'special condition' that distinguishes flares that are accompanied by metric Type II radio bursts from those of comparable size that are not. The leading candidates for this special condition are: (1) an unusually low Alfvén speed in the flaring region; and (2) fast material motion. We present evidence based on SMM and GOES X-ray data and Solwind coronagraph data that argues against the first of these hypotheses and supports the second. Type II bursts linked to flares within 30° of the solar limb are well associated (64%; 49/76) with fast (>400 km s^–1) coronal mass ejections (CMEs); for Type II flares within 15° of the limb, the association rate is 79% (30/38). An examination of the characteristics of 'non-CME' flares associated with Type IIs does not support the flare-initiated blast wave picture that has been proposed for these events and suggests instead that CMEs may have escaped detection. While the degree of Type II–CME association increases with flare size, there are notable cases of small Type II flares whose outstanding attribute is a fast CME. Thus we argue that metric Type II bursts (as well as the Moreton waves and kilometric Type II bursts that may accompany them) have their root cause in fast coronal mass ejections.     

A CME mass distribution derived from SOLWIND coronagraph observations

Using estimates of the masses of nearly 1000 CMEs observed by SOLWIND from Howardet al. (1985), we re-plot the numbers of CMEs as a function of CME mass on a log-linear plot. The plot is significant in that it shows a linear trend over more than a decade of CME masses. The plot indicates a simple form for the distribution of the CME masses and allows an easy determination of the total mass ejected into the solar wind in the form of CMEs. We find that approximately 16% of the solar wind at solar maximum can be comprised of CME mass. There is no indication that the numbers of low-mass CMEs increase in number above the trend set by the more massive ones. Specifically, there is no increase in the numbers of small CMEs such that the whole of the solar wind can be comprised of them.     

Sunspot velocity correlations: Are they due to Reynolds stresses or to the Coriolis force on rising flux tubes?

Observations have consistently pointed out that the longitudinal and latitudinal motions of sunspots are correlated. The magnitude of the covariance was found to increase with latitude, and its sign was found to be positive in the N-hemisphere and negative in the S-hemisphere. This correlation was believed to be due to the underlying turbulence where the sunspot flux tubes are anchored, and the covariance had the right sign and magnitude needed to explain the transfer of angular momentum toward the equator through Reynolds stresses.Here we present an alternate explanation for these sunspot velocity correlations: It is believed that the dynamo operates in a thin overshoot layer beneath the base of the convection zone, and the flux tubes generated there produce sunspots at the photosphere. By studying the dynamics of flux tubes emerging from the base of the convection zone to the photosphere, we show that these velocity correlations of sunspots could be merely a consequence of the effect of Coriolis force on rising flux tubes. The effect of the Coriolis force, as demonstrated by even a back-of-the-envelope calculation, is to push the faster rotating spots equatorward and the slower rotating spots poleward, giving rise to a correlation in their longitudinal and latitudinal velocities, which is positive in the N-hemisphere and negative in the S-hemisphere. The increase in the correlation with latitude is due to the increase in magnitude of the Coriolis force. Hence we show that these velocity correlations might have nothing to do with the Reynolds stresses of the underlying turbulence.We present analyses of observations, and show that the covariances of plages are an order of magnitude higher than the sunspot covariances. If plages and sunspots share the same origin, and if their horizontal velocity correlations are wholly due to the effect of Coriolis force on rising flux tubes, then the study of their dynamics suggests that the flux tubes that form plages should have diameters of a couple of thousand km at the base of the convection zone and remain intact until they reach the photosphere, whereas sunspots should be formed by a collection of small flux tubes (each measuring about a hundred km in diameter), that rise through the convection zone as individual elements and coalesce when they emerge through the photosphere.Operated by the Association of Universities for Research in Astronomy, Inc., under Cooperative Agreement with the National Science Foundation.