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21.
The results of radial velocity measures of the star o And from high dispersion plates relative to the years 1964, 1966, 1975 and 1976 are given. The averaged values of the 1964 and 1966 plates confirm the existence of the minimum in the trend of the radial velocities and fit well the curve obtained in the hypothesis of periodic long-term radial velocity variations with the period of 23.5 years (Fracassiniet al., 1977). Preliminary orbital elements in the hypothesis of a long period spectroscopic binary system have been tentatively drawn.  相似文献   
22.
Late Pliocene–Pleistocene tectonic evolution of the Apennines is driven by progressive eastward migration of extensional downfaulting superposed onto the Late Miocene–Early Pliocene compressional thrust belt. This process has led to distinct structural domains that show decreasing transcrustal permeability from conditions of pervasive mixing between deep and surface fluids in the hinterland (west) to conditions of restricted fluid circulation and overpressuring in the foreland (east). At present, the highest rates of normal faulting and the strongest seismicity occur in the area bounded by stretched, highly permeable crust to the west and thick, poorly permeable crust to the east. In this area, the seismogenic sources of the largest earthquakes (5<Ms<7) are potentially related to mature normal faults that deeply penetrate thick brittle upper crust, and act as transient high-permeability channels during seismic activity. In this framework, it is plausible that domains of overpressuring govern progressive inception of normal faulting and fluid redistribution in the crust, leading to eastward migration of the belt of maximum seismicity with time.  相似文献   
23.
The seismic hazard of Sannio-Matese is calculated using a new seismogenetic zoning of southern Italy of seven areas and different, azimuth-dependent, attenuation laws. Various approaches (Gumbel's first and third asymptotic distribution, Cornell) lead to similar results for the different exposure times considered (100 and 200 years) and probability levels (37 and 68%). The present seismic regulation proposed in 1980 by the Italian National Council for Researches, and based on a different approach, is, in general, confirmed by the results.  相似文献   
24.
We employ our semi-empirical kinematic model for shear body waves (KF) [Sirovich L. A simple algorithm for tracing out synthetic isoseismals. Bull Seism Soc Am 1996;86(4):1019–27; Sirovich L. Synthetic isoseismals of three earthquakes in California-Nevada. Soil Dyn Earthquake Eng 1997;16:353–62] to back-predict and then validate the regional intensity scenario of a destructive earthquake (Loma Prieta, California, Ms 7.1, October 17, 1989). Only the pre-1988 geological and seismotectonic knowledge was used to set the 11 source parameters of KF (in this sense, our procedure was deterministic). Then, the ranges of the pre-1988 uncertainties were explored by grid search and the parametric combination produced 59,049 sources. The quality of our prediction was measured using the field intensities of 1989 by the US Geological Survey (in the MMI scale). The squared scenario residuals are: 73 for the mean KF scenario and 123 for the best available empirical attenuation of MMI intensity. We stress that, before using KF in the forward mode, its automatic inverse application has already been validated by refinding a series of earthquake sources [Gentile F, Pettenati F, Sirovich L. Validation of the automatic nonlinear source inversion of the US geological survey intensities of the Whittier Narrows, 1987 Earthquake. Bull Seism Soc Am 2004;94(5):1737–47; Pettenati F, Sirovich L. Intensity-based source inversion of three destructive California earthquakes. Bull Seism Soc Am 2007;97(5):1587–606; Sirovich L, Pettenati F. Source inversion of intensity patterns of earthquakes: a destructive shock in 1936 in northeast Italy. J Geophys Res 2004;109:B10309, doi:10.1029/2003JB002919:1–16]. If our technique had been available at the time, the 1989 pattern of damage south of San Francisco would have been conservatively foreseen even from 1983 on.  相似文献   
25.
This paper extends our previous study of planet/brown dwarf accretion by giant stars to solar-mass stars located on the red giant branch. The model assumes that the planet is dissipated at the bottom of the convective envelope of the giant star. The evolution of the giant is then followed in detail. We analyse the effects of different accretion rates and different initial conditions. The computations indicate that the accretion process is accompanied by a substantial expansion of the star, and, in the case of high accretion rates, hot bottom burning can be activated. The possible observational signatures that accompany the engulfing of a planet are also extensively investigated. They include the ejection of a shell and a subsequent phase of IR emission, an increase in the 7Li surface abundance and a potential stellar metallicity enrichment, spin-up of the star because of the deposition of orbital angular momentum, the possible generation of magnetic fields and the related X-ray activity caused by the development of shear at the base of the convective envelope, and the effects on the morphology of the horizontal branch in globular clusters. We propose that the IR excess and high Li abundance observed in 4–8 per cent of the G and K giants originate from the accretion of a giant planet, a brown dwarf or a very low-mass star.  相似文献   
26.
We investigate the migration of massive extrasolar planets caused by gravitational interaction with a viscous protoplanetary disc. We show that a model in which planets form at 5 au at a constant rate, before migrating, leads to a predicted distribution of planets that is a steeply rising function of log( a ), where a is the orbital radius. Between 1 and 3 au, the expected number of planets per logarithmic interval in a roughly doubles. We demonstrate that, once selection effects are accounted for, this is consistent with current data, and then extrapolate the observed planet fraction to masses and radii that are inaccessible to current observations. In total, approximately 15 per cent of stars targeted by existing radial velocity searches are predicted to possess planets with masses  0.3< M p sin( i )<10 M J  and radii  0.1< a <5 au  . A third of these planets (around 5 per cent of the target stars) lie at the radii most amenable to detection via microlensing. A further  5–10  per cent of stars could have planets at radii of  5< a <8 au  that have migrated outwards. We discuss the probability of forming a system (akin to the Solar system) in which significant radial migration of the most massive planet does not occur. Approximately  10–15  per cent of systems with a surviving massive planet are estimated to fall into this class. Finally, we note that a smaller fraction of low-mass planets than high-mass planets is expected to survive without being consumed by the star. The initial mass function for planets is thus predicted to rise more steeply towards small masses than the observed mass function.  相似文献   
27.
Metallicity, planetary formation and migration   总被引:1,自引:0,他引:1  
Recent observations show a clear correlation between the probability of hosting a planet and the metallicity of the parent star. As radial velocity surveys are biased, however, towards detecting planets with short orbital periods, the probability–metallicity correlation could merely reflect a dependence of migration rates on metallicity. We investigated the possibility, but find no basis to suggest that the migration process is sensitive to the metallicity. The indication is, therefore, that a higher metallicity results in a higher probability for planet  formation .  相似文献   
28.
Zusammenfassung Die quartären tektonischen Bewegungen in Sizilien waren in ihrem Stil und ihrer Amplitude in den einzelnen Zonen unterschiedlich. Diese Zonen decken sich mit bestimmten paläogeographischen Einheiten. Die marinen Ablagerungen des Calabrien sind teilweise schwach gefaltet, teilweise nur geneigt. Die Verstellung des marinen Quartär ist dort am stärksten, wo auch das Pliozän selbst kräftiger disloziert war. Auf dem Plateau von Syracus, einer deutlich abgegrenzten paläogeographischen Einheit, erreicht das Pliozän nur eine Höhe von 150 m, während Calabrien und Sicilien unbekannt sind.  相似文献   
29.
The possible origin or coherent oscillations in X-ray bursters is discussed. Such oscillations with a period of the order of 10 ms have recently been observed. At this point it seems impossible to draw final conclusions on their nature. Nevertheless, it is shown that nonradial pulsations of a neutron star or torsional oscillations of a neutron star's crust seem to be an attractive possibility.  相似文献   
30.
In the Central Apennines (Italy) three major domains can be recognized: the Umbria and Marche pelagic domains and the Lazio-Abruzzi carbonate platform. Their Mesozoic-Tertiary sequences are separated by major low-angle thrust systems, which superpose the Umbria domain onto both the Marche and Lazio-Abruzzi domains, the Lazio-Abruzzi platform onto the Marche sequence, and all of them onto the Apulia foreland.From Lias to Cretaceous times the Lazio-Abruzzi platform was a fault-controlled uplifted domain separating the Umbria basin to the west from the Marche basin to the east, but closed to the north. The Umbria and Marche basins evolved distinctly with the onset of the terrigenous infilling, beginning with the Serravallian-Tortonian «Marnoso-Arenacea» Formation in the inner Umbria basin and with the Messinian-Early Pliocene Laga Flysch in the outer Marche basin. From Tortonian till Early Pliocene times there was a progressive deformation of the Umbria sequence, with its emplacement onto the Lazio-Abruzzi platform, and the deformation of the Lazio-Abruzzi and Marche zones. In Early-Middle Pliocene times, both the Umbria and Lazio-Abruzzi domains were emplaced onto the previously deformed Marche domain, with passive transport of that portion of Umbria stacked on top of the Lazio-Abruzzi platform. The final stages in Middle-Late Pliocene times caused further motion of the Lazio-Abruzzi platform along the arc-shaped Gran Sasso-Morrone thrust front. Folding and thrusting persisted in the outermost zones till Early Pleistocene times.This reconstruction means that in this area the model of a regularly forward migrating fold-thrust belt is not applicable. It also suggests a large northward displacement of the Lazio-Abruzzi platform, whose differential advancement may be dynamically related to a left-lateral discontinuity to the west and a right-lateral discontinuity to the east. According to our interpretation, the left-lateral discontinuity is not coincident with the «Ancona-Anzio» line of the Italian literature, but rather is buried underneath the Umbria stacked sequences.
Zusammenfassung Der Zentralappennin (Italien) besteht aus drei Hauptbereichen: die pelagialen Gebiete Umbriens und der Marche sowie die Karbon-Platte Latiums und der Abruzzen. Die Formationsgruppen des Mesozoikum-Tertiär dieser drei Gebiete werden durch große Überschiebungsbahnen getrennt, welche die umbrische Zone auf die Zone der Marche sowie Latiums und der Abruzzen schieben, die Zone Latiums und der Abruzzen ihrerseits auf die Formation der Marche und alle zusammen auf das Vorland Apuliens.Die ursprüngliche paleogeographische Struktur der drei Gebiete läßt darauf schließen, daß die Latium-Abruzzen-Platte vom Lias bis zur Kreidezeit eine aktive, erhobene Zone darstellt, die das Umbrische Becken im Westen vom Becken der Marche im Osten trennt, wobei sich die Platte nach Norden hin schließt, was ein Ineinandergreifen der beiden pelagialen Gebiete mit sich bringt. Beide Becken weisen eine getrennte Evolution auf, mit dem Beginn einer terrigenen Zufuhr, bestehend aus der Marnoso-Arenacea-Formation des Serravall-Tortons im Inneren des Umbrischen Beckens und mit dem Laga Flysch des Messin und Unter-Pliozän im äußeren Umbrischen Becken. Vom Torton bis zum Unteren Pliozän hat eine progressive Deformation der Umbrischen Sequenz stattgefunden, die auf dem Gebiete Latiums und der Abruzzen abgelagert wurde, was wiederum zur Deformation in der Zone Latiums und der Abruzzen sowie der Marche führte. Im unteren Mittel-Pliozän wurden sowohl die Formationen Umbriens als auch die der Zonen von Latium und der Abruzzen auf die schon deformierte Formationsgruppe der Marche aufgeschoben, mit nachfolgend passivem Transport des schon auf der Latium-Abruzzen-Platte aufgelagerten Teils der Umbrischen Formation. Die letzten Ereignisse im mittleren Ober-Pliozän führten zu einem weiteren Vorschub der Latium-Abruzzen-Platte längs der bogenförmigen Verwerfungsfront Gran Sasso-Morrone, sowie zu nachfolgenden Falten und Verwerfungen in den äußersten Gebieten bis zum unteren Pleistozän.Diese Rekonstruktion bedeutet vor allen Dingen, daß in diesem Gebiet das Modell einer regelmäßig voranschreitenden Überschiebungsfront nicht anwendbar ist. Sie deutet ferner auf eine große, nordwärts gerichtete Verschiebung der Latium-Abruzzen-Platte hin, deren differenzierter Vorschub dynamisch in Bezug zu einer links-lateralen Verschiebung nach Westen und einer rechts-lateralen Verschiebung nach Osten zu bringen ist. Gemäß unserer Auslegung stimmt die links-laterale Verschiebung nicht mit der «Ancona-Anzio» Linie der einschlägigen italienischen Fachliteratur überein, sondern ist eher unter den überlagernden Sequenzen Umbriens zu suchen.

Résumé On peut distinguer trois domaines dans la partie centrale des Apennins (Italie): le domaine pélagique des Marches, celui de l'Ombrie et la plate-forme carbonatée du Latium-Abruzzes. Les séries stratigraphiques mésozoïques-tertiaires de ces trois domaines sont séparées par d'importants systèmes de chevauchement qui ont provoqué la superposition du domaine ombrien sur ceux des Marches et du Latium-Abruzzes, la superposition de la plate-forme du Latium-Abruzzes sur la série des Marches, et enfin la superposition de toute la chaîne sur l'avantpays de l'Apulie.Du Lias au Crétacé, la plate-forme du Latium-Abruzzes constituait un domaine soulevé par des failles actives; ce domaine séparait le bassin de l'Ombrie à l'ouest du bassin des Marches à l'est et était limité au nord, permettant ainsi la communication des deux régions pélagiques. Ces deux bassins ont présenté une évolution distincte débutant par un remplissage terrigène; celui-ci est représenté, dans le bassin ombrien plus interne par la Formation Marnoso-Arénacéa (Serravalien-Tortonien), et dans le bassin externe des Marches par la formation du Flysch de la Laga (Messinien-Pliocène inférieur). A partir du Tortonien jusqu'au début du Pliocène, la série ombrienne a subi une déformation progressive, et à été charriée sur le domaine du Latium-Abruzzes, provoquant la déformation de ce dernier, ainsi que du domaine des Marches. Au cours du Pliocène inférieur et moyen, les domaines de l'ombrie et du Latium-Abruzzes ont été charriés sur la série des Marches ainsi déformée, entraînant de ce fait le transport passif de la portion de la séquence ombrienne préalablement charriée sur la plate-forme du Latium-Abruzzes. Plus tard, des mouvements méso- à tardi-pliocènes ont provoqué un dernier charriage de la plate-forme du Latium-Abruzzes le long de l'arc de chevauchement Gran Sasso-Morrone; enfin, les plissements et les charriages ont persisté dans les zones les plus externes jusqu'au Pléistocène inférieur.Cette reconstitution signifie que le modèle d'une chaîne plissée et charriée se déplaçant régulièrement vers l'avant-pays ne peut pas être appliqué à cette région. Elle indique également un vaste déplacement vers le Nord de la plate-forme du Latium-Abruzzes, transport qui peut être dynamiquement mis en relation avec un décrochement sénestre à l'ouest et un décrochement dextre à l'est. Selon notre interprétation, le décrochement sénestre ne coïncide pas avec la ligne «Ancona-Anzio» de la littérature italienne, mais est enterré sous l'édifice charrié de l'Ombrie.

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