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1.
Fabio Speranza Patrizia Landi Francesca D’Ajello Caracciolo Alessandro Pignatelli 《Bulletin of Volcanology》2010,72(7):847-858
We report on the paleomagnetism of ten sites in the products of the most recent silicic eruptive cycle of Pantelleria, Strait
of Sicily. Previously radiometrically dated at 5–10 ka, our comparison with proxies for geomagnetic field directions allows
us to narrow considerably the time window during which these eruptions occurred. The strongly peralkaline composition causes
the magmas to have low viscosities, locally resulting in strong agglutination of proximal fall deposits. This allows successful
extraction of paleomagnetic directions from the explosive phases of eruptions. One of our sites was located in the Serra della
Fastuca fall deposit, produced by the first explosive event of the eruptive cycle. The other nine sites were located in the
most recent explosive (pumice fall and agglutinate from Cuddia del Gallo and Cuddia Randazzo) and effusive (Khaggiar lava)
products. The (very similar) paleomagnetic directions gathered from eight internally consistent sites were compared to reference
geomagnetic field directions of the last 5–10 ka. Directions from Cuddia del Gallo agglutinate and Khaggiar flows translate
into 5.9- to 6.2-ka ages, whereas the Fastuca pumices yield a slightly older age of 6.2–6.8 ka. Hence, the most recent silicic
eruptive cycle lasted at most a millennium and as little as a few centuries around 6.0 ka. Paleomagnetically inferred ages
are in good agreement with published (and calibrated by us) 14C dates from paleosols/charcoals sampled below the studied volcanic units, whereas K/Ar data are more scattered and yield
∼30% older ages. Our data show that the time elapsed since the most recent silicic eruptions at Pantelleria is comparable
to the quiescence period separating the two latest volcanic cycles. 相似文献
2.
E. Pignatelli 《Astrophysics and Space Science》2001,276(2-4):483-489
We present an application of a new set of detailed, self-consistent, dynamical models for disc galaxies. We start from the
hypothesis that each galaxy can be decomposed into a bulge, following the r
1/4law, and a disc with an exponential projected density profile; and that the isodensity surfaces of each component can be represented
by similar concentric spheroids. After taking into account both the asymmetric drift effects and the integration along the
line of sight, we produce the rotational velocity and velocity-dispersion profile, andthe approximate shape of the line-of-sight velocity distributions for the stars as parameterized by the h
3 and h
4 coefficients of theGauss–Hermite expansion of the line profile. Photometric and kinematical data have been taken from the
literature for the test case of the S0 galaxy NGC 5866, for which detailed stellar kinematical data are available at different
positions across the galaxy. Apart from the innermost, dust-obscured regions of the galaxy, where observational effects are
likely to be dominant, the model successfully reproduces the whole set of dynamical data available as well as giving a good
fit to the photometry. The galaxy is shown to have an isotropic velocity-dispersion tensor, thus hinting at a dissipational
formation process.
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献
3.
Isabella Pignatelli Yves Marrocchi Lionel. G. Vacher Rémi Delon Matthieu Gounelle 《Meteoritics & planetary science》2016,51(4):785-805
We report a petrographic and mineralogical survey of tochilinite/cronstedtite intergrowths (TCIs) in Paris, a new CM chondrite considered to be the least altered CM identified to date. Our results indicate that type‐I TCIs consist of compact tochilinite/cronstedtite rims surrounding Fe‐Ni metal beads, thus confirming kamacite as the precursor of type‐I TCIs. In contrast, type‐II TCIs are characterized by complex compositional zoning composed of three different Fe‐bearing secondary minerals: from the outside inwards, tochilinite, cronstedtite, and amakinite. Type‐II TCIs present well‐developed faces that allow a detailed morphological analysis to be performed in order to identify the precursors. The results demonstrate that type‐II TCIs formed by pseudomorphism of the anhydrous silicates, olivine, and pyroxene. Hence, there is no apparent genetic relationship between type‐I and type‐II TCIs. In addition, the complex chemical zoning observed within type‐II TCIs suggests that the alteration conditions evolved dramatically over time. At least three stages of alteration can be proposed, characterized by alteration fluids with varying compositions (1) Fe‐ and S‐rich fluids; (2) S‐poor and Fe‐ and Si‐rich fluids; and (3) S‐ and Si‐poor, Fe‐rich fluids. The presence of unaltered silicates in close association with euhedral type‐II TCIs suggests the existence of microenvironments during the first alteration stages of CM chondrites. In addition, the absence of Mg‐bearing secondary minerals in Paris TCIs suggests that the Mg content increases during the course of alteration. 相似文献
4.
R. Carluccio A. Giuntini V. Materni S. Chiappini C. Bignami F. D’Ajello Caracciolo A. Pignatelli S. Stramondo R. Console M. Chiappini 《Pure and Applied Geophysics》2014,171(3-5):341-359
The Democratic People Republic of Korea announced two underground nuclear tests carried out in their territory respectively on October 9th, 2006 and May 25th, 2009. The scarce information on the precise location and the size of those explosions has stimulated various kinds of studies, mostly based on seismological observations, by several national agencies concerned with the Nuclear Test Ban Treaty verification. We analysed the available seismological data collected through a global high-quality network for the two tests. After picking up the arrival times at the various stations, a standard location program has been applied to the observed data. If we use all the available data for each single event, due to the different magnitude and different number of available stations, the locations appear quite different. On the contrary, if we use only the common stations, they happen to be only few km apart from each other and within their respective error ellipses. A more accurate relative location has been carried out by the application of algorithms such as double difference joint hypocenter determination (DDJHD) and waveform alignment. The epicentral distance between the two events obtained by these methods is 2 km, with the 2006 event shifted to the ESE with respect to that of 2009. We then used a dataset of VHR TerraSAR-X satellite images to detect possible surface effects of the underground tests. This is the first ever case where these highly performing SAR data have been used to such aim. We applied InSAR processing technique to fully exploit the capabilities of SAR data to measure very short displacements over large areas. Two interferograms have been computed, one co-event and one post-event, to remove possible residual topographic signals. A clear displacement pattern has been highlighted over a mountainous area within the investigated region, measuring a maximum displacement of about 45 mm overall the relief. Hypothesizing that the 2009 nuclear test had been carried out close to the area where the displacement has been observed through the DInSAR technique, its relation with the epicenter location obtained through seismological processing has been discussed as a possible alternative hypothesis with respect to the preferred solutions reported by the nuclear explosion database (NEDB). The distance of about 10 km between the two places can be considered acceptable in light of the possible systematic location shifts commonly observed in the seismological practice over a global scale. The difference between the m b magnitudes of the two tests could reflect differences in geological conditions of the two test sites, even if the yield of the two explosions had been the same. 相似文献
5.
Pignatelli Alessandro D’Ajello Caracciolo Francesca Console Rodolfo 《Journal of Seismology》2021,25(6):1347-1359
Journal of Seismology - Analyzing seismic data to get information about earthquakes has always been a major task for seismologists and, more in general, for geophysicists. Recently, thanks to the... 相似文献
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7.
Régine?Mosser-RuckEmail author Isabella?Pignatelli Franck?Bourdelle Mustapha?Abdelmoula Odile?Barres Damien?Guillaume Delphine?Charpentier Davy?Rousset Michel?Cathelineau Nicolas?Michau 《Contributions to Mineralogy and Petrology》2016,171(11):97
The smectite-to-chlorite conversion is investigated through long-duration experiments (up to 9 years) conducted at 300 °C. The starting products were the Wyoming bentonite MX80 (79 % smectite), metallic iron and magnetite in contact with a Na–Ca chloride solution. The predominant minerals in the run products were an iron-rich chlorite (chamosite like) and interstratified clays interpreted to be chlorite/smectite and/or corrensite/smectite, accompanied by euhedral crystals of quartz, albite and zeolite. The formation of pure corrensite was not observed in the long-duration experiments. The conversion of smectite into chlorite over time appears to take place in several steps and through several successive mechanisms: a solid-state transformation, significant dissolution of the smectite and direct precipitation from the solution, which is over-saturated with respect to chlorite, allowing the formation of a chamosite-like mineral. The reaction mechanisms are confirmed by X-ray patterns and data obtained on the experimental solutions (pH, contents of Si, Mg, Na and Ca). Because of the availability of some nutrients in the solution, total dissolution of the starting smectite does not lead to 100 % crystallization of chlorite but to a mixture of two dominant clays: chamosite and interstratified chlorite/smectite and/or corrensite/smectite poor in smectite. The role of Fe/(Fe + Mg) in the experimental medium is highlighted by chemical data obtained on newly formed clay particles alongside previously published data. The newly formed iron-rich chlorite has the same composition as that predicted by the geothermometer for diagenetic to low-grade metamorphic conditions, and the quartz + Fe-chlorite + albite experimental assemblage in the 9-year experiment is close to that fixed by water–rock equilibrium. 相似文献
8.
Ezio Pignatelli Paolo Salucci Luigi Danese 《Monthly notices of the Royal Astronomical Society》2001,320(1):124-130
In this work we build a detailed dynamic model for an S0 galaxy possibly hosting a central massive dark object (MDO). We show that the photometric profiles and the kinematics along the major and minor axes, including the h 3 and h 4 profiles, imply the presence of a central MDO of mass i.e. 0.3–2.8 per cent of the mass derived for the stellar spheroidal component. Models without MDO are unable to reproduce the kinematic properties of the inner stars and of the rapidly rotating nuclear gas.
The stellar population consists of an exponential disc (27 per cent of the light) and a diffuse spheroidal component (73 per cent of the light) that cannot be represented by a simple de Vaucouleurs profile at any radius. The M L ratios we found for the stellar components (3.3 and 6.6 respectively) are typical of those of disc and elliptical galaxies. 相似文献
The stellar population consists of an exponential disc (27 per cent of the light) and a diffuse spheroidal component (73 per cent of the light) that cannot be represented by a simple de Vaucouleurs profile at any radius. The M L ratios we found for the stellar components (3.3 and 6.6 respectively) are typical of those of disc and elliptical galaxies. 相似文献
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E. Pignatelli E. M. Corsini J. C. Vega Beltrán C. Scarlata A. Pizzella J. G. Funes S. J. W. W. Zeilinger J. E. Beckman F. Bertola 《Monthly notices of the Royal Astronomical Society》2001,323(1):188-210
We present V -band surface photometry and major-axis kinematics of stars and ionized gas of three early-type spiral galaxies, namely NGC 772, 3898 and 7782. For each galaxy we present a self-consistent Jeans model for the stellar kinematics, adopting the light distribution of bulge and disc derived by means of a two-dimensional parametric photometric decomposition. This allows us to investigate the presence of non-circular gas motions, and derive the mass distribution of luminous and dark matter in these objects.
NGC 772 and 7782 have apparently normal kinematics with the ionized gas tracing the gravitational equilibrium circular speed. This is not true in the innermost region (| r |≲8 arcsec) of NGC 3898, where the ionized gas is rotating more slowly than the circular velocity predicted by dynamical modelling. This phenomenon is common in the bulge-dominated galaxies for which dynamical modelling enables us to make the direct comparison between the gas velocity and the circular speed, and it poses questions about the reliability of galaxy mass distributions derived by the direct decomposition of the observed ionized-gas rotation curve into the contributions of luminous and dark matter. 相似文献
NGC 772 and 7782 have apparently normal kinematics with the ionized gas tracing the gravitational equilibrium circular speed. This is not true in the innermost region (| r |≲8 arcsec) of NGC 3898, where the ionized gas is rotating more slowly than the circular velocity predicted by dynamical modelling. This phenomenon is common in the bulge-dominated galaxies for which dynamical modelling enables us to make the direct comparison between the gas velocity and the circular speed, and it poses questions about the reliability of galaxy mass distributions derived by the direct decomposition of the observed ionized-gas rotation curve into the contributions of luminous and dark matter. 相似文献