Environmental Effects in Galaxies: Molecular Gas and Nuclear Activity

Galactic X-ray emitters have been described by Giovannelli andSabau-Graziati (1993). We would address the bulk of this paper on HighMass X-Ray Binaries (HMXBs) and particularly in demonstrating theimportance of these systems as powerful laboratories to test the propertiesof high-energy physical processes through the multi-frequency studies oftheir behavior. Interactions between the two components of those systemsoriginate processes that manifest themselves along a large part of theelectromagnetic spectrum. Therefore it is possible to study indirectlyhigh-energy phenomena through the analysis oflow-energy phenomena with enormous advantages since the latter can bemainly studied via ground-based experiments, meanwhile the former can bestudied only by mean of space-based experiments, at least up to energiesof order 100 GeV.Moreover, since HMXBs are galactic, their emissions are the highestmeasurable; this renders such systems the most powerful laboratories to testtheories on collapsed objects, which can be scaled to extra-galactic distancesand dimensions. This fact suggests that HMXBs can be in general useful targetseven for small satellites, and in particular, in the X-ray energy range,very suitable targets for experiments like SIXE (Spanish Italian X-rayExperiment) to be launched in small satellites such as the Spanish MINISAT-02.     

Polycyclic aromatic hydrocarbon lifetime in cometary environments

Observations of cometary comae in the infrared and in the near-ultraviolet suggest that polycyclic aromatic hydrocarbons (PAHs) are present in these environments. However, the chemical identity and abundance of these molecules are not clearly determined yet. Some species are probably more stable than others when submitted to the solar radiation field, and are therefore more likely to be observed. The photophysics of gas-phase PAHs in cometary environments is modelled. Photodissociation occurs when the heating by absorption of UV photons is more efficient than the radiative cooling. The lifetime of the molecules is found to depend on their size: small molecules being more stable than large ones. Furthermore, at 1 AU from the Sun, the lifetime of PAHs is found to be very short (20s for phenanthrene). This suggests that, if observed in the gas phase in cometary environments, these molecules should be produced by an extended source.     

Vegetation history and environmental development since ca 6000 cal yr BP in and around Ispani 2 (Kolkheti lowlands,Georgia)

The Kolkheti lowlands of western Georgia have a unique vegetation and a rich cultural history. Palynological and macrofossil analysis accompanied by AMS ¹⁴C-dates of the deposits of the Ispani 2 mire near Kobuleti allow the reconstruction of regional vegetation, environmental history and local peatland development within the context of Black Sea level and cultural changes. Comparison of two adjacent peatland cores confirms spatial differences in wetland development. Prior to 5400 cal yr BP, the Ispani basin was a floodplain of an active river system where overbank deposits with fluvially transported Castanea pollen were deposited. Subsequently, a lake or lagoon developed in which reeds expanded. These were succeeded by herb-rich open alder carrs. After 1900 cal yr BP, Carpinus and Fagus expanded on the dry grounds, where formerly Quercus was more abundant. Also Castanea declined. Local reedbeds, that burned regularly, succeeded the alder carr. After 1000 cal yr BP, a percolation bog developed resulting in the formation of 4 m of loose, porous, and largely undecomposed Sphagnum austinii peat with Molinia roots. The upper 50 cm of the analysed section show extensive human impact on the landscape during the 20th century.     

A Measurement of Omega from the North American Test Flight of Boomerang

We use the angular power spectrum of the cosmic microwave background, measured during the North American test flight of the Boomerang experiment, to constrain the geometry of the universe. Within the class of cold dark matter models, we find that the overall fractional energy density of the universe Omega is constrained to be 0.85相似文献   

Speckle imaging of Titan at 2 microns: surface albedo, haze optical depth, and tropospheric clouds 1996-1998

We present results from 14 nights of observations of Titan in 1996-1998 using near-infrared (centered at 2.1 microns) speckle imaging at the 10-meter W.M. Keck Telescope. The observations have a spatial resolution of 0.06 arcseconds. We detect bright clouds on three days in October 1998, with a brightness about 0.5% of the brightness of Titan. Using a 16-stream radiative transfer model (DISORT) to model the central equatorial longitude of each image, we construct a suite of surface albedo models parameterized by the optical depth of Titan's hydrocarbon haze layer. From this we conclude that Titan's equatorial surface albedo has plausible values in the range of 0-0.20. Titan's minimum haze optical depth cannot be constrained from this modeling, but an upper limit of 0.3 at this wavelength range is found. More accurate determination of Titan's surface albedo and haze optical depth, especially at higher latitudes, will require a model that fully considers the 3-dimensional nature of Titan's atmosphere.     

Keck near-infrared observations of Saturn's E and G rings during Earth's ring plane crossing in August 1995

We present near-infrared (1.24-2.26 μm) images of Saturn's E and G rings which were taken with the W.M. Keck telescope in 1995 August 9-11, during the period that Earth crossed Saturn's ring plane. Our data confirm that the E ring is very blue. Its radial and vertical structure are found to be remarkably similar to that apparent in the HST ringplane crossing data at visible wavelengths, reinforcing models of the ring's peculiar narrow or very steep particle size distribution. Our data show unambiguously that the satellite Tethys is a secondary source of material for the E ring. The G ring is found to be distinctly red, similar in color to Jupiter's main ring, indicative of a (more typical) broad particle size distribution.