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491.
Generoso Aliasi Giovanni Mengali Alessandro A. Quarta 《Celestial Mechanics and Dynamical Astronomy》2011,110(4):343-368
This paper introduces a new approach to the study of artificial equilibrium points in the circular restricted three-body problem
for propulsion systems with continuous and purely radial thrust. The propulsion system is described by means of a general
mathematical model that encompasses the behavior of different systems like a solar sail, a magnetic sail and an electric sail.
The proposed model is based on the choice of a coefficient related to the propulsion type and a performance parameter that
quantifies the system technological complexity. The propulsion system is therefore referred to as generalized sail. The existence
of artificial equilibrium points for a generalized sail is investigated. It is shown that three different families of equilibrium
points exist, and their characteristic locus is described geometrically by varying the value of the performance parameter.
The linear stability of the artificial points is also discussed. 相似文献
492.
Giacomo BRIANI Alessandro MORBIDELLI Matthieu GOUNELLE David NESVORNÝ 《Meteoritics & planetary science》2011,46(12):1863-1877
Abstract– Micrometeoroids with 100 and 200 μm size dominate the zodiacal cloud dust. Such samples can be studied as micrometeorites, after their passage through the Earth atmosphere, or as microxenoliths, i.e., submillimetric meteorite inclusions. Microxenoliths are samples of the zodiacal cloud dust present in the asteroid Main Belt hundreds of millions years ago. Carbonaceous microxenoliths represent the majority of observed microxenoliths. They have been studied in detail in howardites and H chondrites. We investigate the role of carbonaceous asteroids and Jupiter‐family comets as carbonaceous microxenolith parent bodies. The probability of low velocity collisions of asteroidal and cometary micrometeoroids with selected asteroids is computed, starting from the micrometeoroid steady‐state orbital distributions obtained by dynamical simulations. We selected possible parent bodies of howardites (Vesta) and H chondrites (Hebe, Flora, Eunomia, Koronis, Maria) as target asteroids. Estimates of the asteroidal and cometary micrometeoroid mass between 2 and 4 AU from the Sun are used to compute the micrometeoroid mass influx on each target. The results show that all the target asteroids (except Koronis) receive the same amount (within the uncertainties) of asteroidal and cometary micrometeoroids. Therefore, both these populations should be observed among howardite and H chondrite carbonaceous microxenoliths. However, this is not the case: carbonaceous microxenoliths show differences similar to those existing among different groups of carbonaceous chondrites (e.g., CI, CM, CR) but two sharply distinct populations are not observed. Our results and the observations can be reconciled assuming the existence of a continuum of mineralogical and chemical properties between carbonaceous asteroids and comets. 相似文献
493.
Non-Keplerian orbits for electric sails 总被引:1,自引:0,他引:1
Giovanni Mengali Alessandro A. Quarta 《Celestial Mechanics and Dynamical Astronomy》2009,105(1-3):179-195
An electric sail is capable of guaranteeing the fulfilment of a class of trajectories that would be otherwise unfeasible through conventional propulsion systems. In particular, the aim of this paper is to analyze the electric sail capabilities of generating a class of displaced non-Keplerian orbits, useful for the observation of the Sun’s polar regions. These orbits are characterized through their physical parameters (orbital period and solar distance) and the spacecraft propulsion capabilities. A comparison with a solar sail is made to highlight which of the two systems is more convenient for a given mission scenario. The optimal (minimum time) transfer trajectories towards the displaced orbits are found with an indirect approach. 相似文献
494.
Based on Williams' work and rewritten in action angle variables, a method for the calculation of proper elements is here presented. The averaging over the long periodic terms is performed by the semi numerical method developed by Henrard (1990); no series expansion in eccentricity or inclination of the asteroid is used which allows calculating proper elements for highly inclined orbits. Conversely, the theory is truncated at the first degree in the eccentricity and the inclination of the perturbing planets. A few tests about accuracy and consistency are presented. 相似文献
495.
Alessandro Morbidelli Antonio Giorgilli 《Celestial Mechanics and Dynamical Astronomy》1989,47(2):145-172
The classical problem of the dynamics in the asteroids belt is revisited in the light of recently developed perturbation methods. We consider the spatial problem of three bodies both in the circular and in the elliptic case, looking for families of periodic or quasi periodic orbits. Some criteria for deciding the stability of these families are also indicated. 相似文献
496.
Alessandro Ellero Leonardo Leoni Michele Marroni Ionel Nicolae Luca Pandolfi Franco Sartori 《Comptes Rendus Geoscience》2002,334(5):347-354
The Fenes Nappe belongs to the stack of tectonic units cropping out in the southern Apuseni Mts (Romania). It is characterised by a structural history consisting of two folding phases that developed during the time spanning from Early Aptian to Late Maastrichtian. The D1 phase produced west-northwest-verging, isoclinal to very tight folds, associated to a slaty cleavage. The main metamorphic imprint of the Fenes Nappe is linked to this deformation phase; illite and chlorite ‘crystallinity’ values indicate metamorphic conditions of the late diagenesis, close to the diagenetic zone/anchizone boundary. The subsequent D2 phase produced north-northwest-verging, parallel folds, not associated with synkinematic recrystallisation. These phases are interpreted as developed during a structural path, which includes burial at a depth of 8–10 km, followed by exhumation at shallower structural levels. To cite this article: A. Ellero et al., C. R. Geoscience 334 (2002) 347–354. 相似文献
497.
Aldo Del Moro Paolo Fulignati Paola Marianelli Alessandro Sbrana 《Journal of Volcanology and Geothermal Research》2001,112(1-4)
During the 1944 eruption of Vesuvius different types of xenoliths were ejected. They represent fragments of the walls of a low volume (<0.5 km3) shallow (3–4 km depth) magma chamber. The study of these xenoliths enables us to estimate the amount of contamination occurring at the boundary of a high-T alkaline magma chamber hosted in carbonate rocks. The process of contamination of the magma by carbonates can be modelled, using isotopic and chemical data, as a mixing between magma and marbles. Mass exchanges occur at the boundary between the crystallizing magma and marble wall rocks, where endoskarn forms. The contamination of the solidification front of the chamber is very limited. The solidification front and the skarn shell effectively isolate the interior of the magma chamber from new inputs of contaminants from the carbonate wall rocks. Therefore, the main volume of magma, hosted in the magma chamber, did not undergo any significant mass exchange with the wall rocks. 相似文献
498.
Alessandro Tibaldi 《Bulletin of Volcanology》2001,63(2-3):112-125
This paper demonstrates that four large sector collapses have affected the NW flank of the Stromboli volcano in the past 13 ka, alternating with growth phases, in order to contribute to the evaluation of the critical conditions which trigger lateral collapses, a reconstruction of the geometry of each collapse of the volcano edifice in the four stages that preceded the relative collapse events is also presented, and a computation of the landslide volume. This reconstruction is based on new field data plotted in three dimensions. Prior to the initial 13-ka collapse, the volcano was 1125±100 m high above sea level. The collapse had a volume of 2.23±0.87 km3, whereas the pre-collapse volcano volume was 218.8±7.7 km3. The next edifice that failed was 900±70 m high a.s.l. The collapse volume was 1±0.54 km3, with a precollapse volcano volume of 201.4±5.4 km3. The edifice then grew to 1000±60 m a.s.l. The third collapse had a volume of 1.08±0.39 km3 and occurred within a volcano with a volume of 209.1±4.6 km3. This was followed by a new growth phase followed by the last collapse with a volume of 0.73±0.22 km3. The volcano volume was about the same as the present one. The present active crater zone is at 780 m a.s.l. in the first three collapses, sliding surfaces cut the main magma conduit. In the last collapse, the upper scarp coincided with the conduit location. Dyking along a main NE-trending weakness zone across the volcano summit exerted a lateral force for collapse inception. The decrease of the landslide volumes with the age, and the concentric scarps of the four collapses, suggest that the younger sliding planes tended to become more superficial and to decrease the areal extent. This is interpreted as due to: (a) successively weaker eruptive products from dominantly lavas to dominantly pyroclastics; and (b) the feedback effects between collapses and dykes that injected along the lateral segments of the first collapse slide plane. 相似文献
499.
500.
M. Aglietta B. Alessandro P. Antonioli F. Arneodo L. Bergamasco M. Bertaina A. Campos Fauth A. Castellina C. Castagnoli A. Chiavassa G. Cini B. D'Ettorre Piazzoli G. Di Sciascio W. Fulgione P. Galeotti P. L. Ghia M. Iacovacci G. Mannocchi C. Melagrana C. Morello G. Navarra L. Riccati O. Saavedra G. C. Trinchero P. Vallania S. Vernetto 《Astrophysics and Space Science》1995,231(1-2):351-354
We present the results of a search for Gamma Ray Bursts at energies E 10 GeV and E 100 TeV made by the EAS-TOP Air Shower Array in correlation with 50 events detected by BATSE in the last 3 years.This analysis gives an indication of the sensitivity of air shower arrays in the detection of GRBs at energies beyond the range seen by satellite experiments. 相似文献