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41.
We present a physical model to explain the existence of a class of large-lightcurve-amplitude, rapidly rotating asteroids found most commonly among objects in the size range 100–300 km diameter. A significant correlation between rotation period and lightcurve amplitude exists for asteroids in this size range in the sense that those with larger amplitudes spin more rapidly and hence these objects have high rotational angular momenta. Since this is a property of Jacobi ellipsoids, we have investigated whether these asteriods might be examples of triaxial equilibrium ellipsoids. We find that objects rotating with periods of 6 hr must have densities between 1.1 and 1.4 g cm?3, while those rotating in 4 hr would have densities between 2.4 and 3.2 g cm?3. If this model is valid then at least some of these asteroids have rather low mean densities. The reality of this result and its interpretation in terms of collisional evolution of the asteroids is discussed. 相似文献
42.
C. Tedesco 《Bulletin of Volcanology》1965,28(1):119-137
Geological investigations were performed on the Roccamonfina extint volcano with the purpose to recognize the nature of the main volcanic formations (with particular regard to pyroclastic deposits) and to ascertain their true order of succession. The volcanic history may be sketched as follows:
- 1)Successive eruptions of mostly leucitic lavas and tuffs build up a normal stratovolcano, about 1700 m high. Several adventive cones, sometimes formed of trachytic lava, rise on its flanks. 相似文献
43.
Results of UBV photometry and polarimetry of 1580 Betulia during its 1976 apparition are presented. The synodic period of rotation is found to be 6.130 hr. The linear phase coefficient and absolute magnitude of the primary maximum in V are 0.032 mag/deg and 14.88, respectively. No color variations with rotation or solar phase angle detected, the mean colors being B?V = 0.66 and U?B = 0.24. Betulia's lightcurve is unique among asteroids studied to date in that it displays three maxima and three minima within one rotational cycle, indicative of a region of greater roughness and/or a dark spot on one of its broad faces. Polarization results indicate a low albedo and a mean diameter of about 7 km, establishing Betulia as the first C type asteroid to be found among the Mars crossers. A model accounting for most features of Betulia's lightcurve is given by a prolate spheroid rotating about one of its shorter axes having an axis ratio of 1:1.21 with a major topographic feature on one of its broad faces. 相似文献
44.
Little is known about potential environmental impact of nanoparticles. Gold nanoparticles can cause unexpected biological responses. Here, Mytilus edulis were exposed (24h) to gold-citrate nanoparticles (GNP), menadione and both compounds simultaneously (GNP/menadione). Protein ubiquitination and carbonylation were determined in gill, mantle and digestive gland, along with traditional oxidative stress biomarkers; catalase activity and neutral red retention time assay (haemolymph). 2DE gels were performed on gill proteins (menadione; GNP/menadione). Our results reveal that GNP may induce oxidative stress. 相似文献
45.
Peter Jenniskens Ed Tedesco Jayant Murthy Christophe O. Laux Stephen Price 《Meteoritics & planetary science》2002,37(8):1071-1078
Abstract— We used the ultraviolet to visible spectrometers onboard the midcourse space experiment to obtain the first ultraviolet spectral measurements of a bright meteor during the 1997 Leonid shower. The meteor was most likely a Leonid with a brightness of about‐2 magnitude at 100 km altitude. In the region between 251 and 310 nm, the two strongest emission lines are from neutral and ionized magnesium. Ionized Ca lines, indicative of a hot T ? 10 000 K plasma, are not detected. The Mg and Mg+ line intensity ratio alone does not yield the ionization temperature, which can be determined only by assuming the electron density. A typical air plasma temperature of T = 4400 K would imply a very high electron density: ne = 2.2 times 1018 m‐3, but at chondritic abundances of Fe/Mg and Si/Mg ? 1. For a more reasonable local‐thermodynamic‐equilibrium (LTE) air plasma electron density, the Mg and Mg+ line ratio implies a less than chondritic Fe/Mg = 0.06 abundance ratio and a cool non‐LTE T = 2830 K ionization temperature for the ablation vapor plasma. The present observations do not permit a choice between these alternatives. The new data provide also the first spectral confirmation of the presence of molecular OH and NO emission in meteor spectra. 相似文献
46.
Albedos for 57 asteroids were determined using diameters obtained from stellar occultations. For 18 objects, the occultation albedos were determined to accuracies better than 5%. The effect on the occultation albedo due to errors in the asteroid absolute magnitude is discussed and correlations between the occultation albedos and IRAS and polarimetric albedos are presented. The higher-quality occultation albedos presented here are suitable for calibrating albedos obtained by indirect methods. 相似文献
47.
Abstract— Important improvements have been made in recent years in understanding the likely origins of near‐Earth objects (NEOs), and extensive observational campaigns are ongoing in order to assess their current inventory. From these studies we can hope to obtain a much better understanding of the different populations of minor bodies, their relationship with meteorites, and the overall history of the solar system. At the same time, NEOs are important also in terms of impact hazard. Both the purely scientific issues, and the more pragmatic point of view focused on the need of developing credible strategies of impact mitigation, require a major effort in order to improve the current knowledge of the physical properties of these objects. 相似文献
48.
Hydrogeochemistry of Roccamonfina volcano (Southern Italy) 总被引:1,自引:1,他引:0
Emilio Cuoco Giuseppe Verrengia Stefano De Francesco Dario Tedesco 《Environmental Earth Sciences》2010,61(3):525-538
This is the first hydro-geochemical investigation carried out on the Roccamonfina Volcanic Complex groundwaters. The chemistry
of Roccamonfina waters is defined by water–rock and water–rock–gas interactions. In fact, interactions between rocks of the
first eruptive high-K formations and circulating groundwaters are recognized by high K concentrations. On the other hand,
inverse concentration of calcium versus alkali metals is related to two different rock interactions occurring in different
areas of the volcano: (a) within the caldera where groundwaters flow within latite and pyroclastic formations releasing calcium,
and (b) similarly at the base of the volcano where groundwaters flowing from surrounding carbonates got strongly enriched
in Ca. These geochemical processes are also associated with K (SE of caldera) and Mg/Ca (in sites located at the NE base of
the volcano) decrease. Completely different dynamics occurs at Riardo groundwaters (SE). Here waters are the result of a mix
between the Roccamonfina deep aquifer and the carbonate aquifer of the Riardo plain. Rich-CO2 emissions make these waters strongly mineralized. Minor elements show a similar geochemical behavior of major ions and are
crucial defining interactions processes. The evolution of Roccamonfina groundwaters is also evident along the simultaneous
enrichment of Ba, Sr, and Ca. Ba increase is the result of deep local carbonate alteration enhanced by CO2 emissions and, the lower Sr/Ca ratio, from 10 to 2 (ppb/ppm), is also due to the same process. In the light of our results
the Roccamonfina aquifer can be schematically divided into two main reservoirs: (a) a superficial aquifer which basically
follows the volcanic structure morphology and tectonics and (b) a deeper reservoir, originating within the oldest Roccamonfina
volcano ultra potassic lavas and then flowing into the carbonate aquifers of the neighboring plain. Eventually, the chemistry
of the Roccamonfina aquifer does not show any specific and visible pollution, contrary to what happens in the volcano surrounding
plains. In fact, only 14% of the samples we collected (206) show a NO3 content >30 mg/l. These sites are all located at the base of the volcano, near the plain. 相似文献
49.
In 1971 asteroid Vesta was observed in a region of the sky in which it had never been observed before. Its photometric lightcurve had two distinct maxima. Those observations have been the only strong evidence to support a rotation period of about 10 hr 41 min. Lightcurves made in 1982, when Vesta was at the same aspect as 1971, do not show two different maxima. It is concluded that there was a systematic error in the 1971 observations. At this time a definitive statement cannot be made about the true period of Vesta, although the 5 hr 20 min period does appear more plausible. Radar echoes in 1988 and 1992 should resolve the problem. The shorter rotation period was assumed and the photometric astrometry method applied. The sidereal period is 5 hr 20 min 31.68 sec 0.2225889 ± 0.0000002 days, the rotation is prograde, and the coordinates of the north pole are 103° longitude and +43° latitude with an uncertainty of abour 6°. 相似文献
50.
JHK infrared photometry shows that R asteroids have two distinct infrared color domains. Most R asteroids have JHK and visual colors and albedos that fall amongst those observed for S asteroids, but a small subset is clearly different. These are designated as a new A class of asteroids. 相似文献