Electron-impact excitation of the Cameron system (a3π → X1Σ)of CO

We have studied the excitation of the Cameron bands of carbon monoxide (a³π → X¹Σ⁺) by electron impact on CO and CO₂. This investigation was prompted by a recent study of the Martian airglow by Conway (1981) who concluded that the cross section for the dissociative excitation of the Cameron bands is seven times larger than the laboratory value reported by Ajello (1971a) and by a perplexing inconsistency between the optical cross section and CO(a³π) time-of-flight experiments. We have found now that three factors have contributed to these discrepancies: (1) spectral contamination of the (1,4) Cameron band used by Ajello to normalize the entire Cameron band cross section, (2) major revisions in the magnitude of the CO(a³π) radiative lifetime, and (3) new insights into the effects of the CO(a³π) velocity distribution on the field of view of the emission experiments. The new results largely reconcile the TOF and emission measurements, but they also suggest that the calculated photoelectron fluxes in the Martian atmosphere may be too large by a factor of 3.     

Chemische und bakteriologische Untersuchungen im unteren Zürichsee während der Jahre 1948–1957

Ohne Zusammenfassung     

Kristallisationsschieferung oder Abbildungskristalloblastese?

Ohne Zusammenfassung     

Synthesis of symmetric flattop radiation patterns

In this communication, the design of ring arrays that produce symmetric flattop radiation patterns with low sidelobes is presented. The equivalent linear array approach is used in the design of the array. A newly developed iterative algorithm is employed to obtain a prototype linear array that generates a desired flattop pattern. A new concept of common scale factor of ring arrays is introduced, which not only adds flexibility to the design, but also reduces the complexity of the array. In the design examples presented, it is shown that an almost flattop pattern with maximum ripple less than 0.075 dB and sidelobe levels less than 28 dB can be achieved using only 10 ring radiators     

TOURISM DEVELOPMENT ON VANCOUVER ISLAND: AN ASSESSMENT OF THE CORE-PERIPHERY MODEL *

This paper examines tourism development on Vancouver Island, B.C. in terms of the core-periphery approach to regional planning. It examines whether a core area (Victoria) is willing to share its tourism business with the rest of the island, and then focuses on the situation in a peripheral region (the Cowichan Valley Regional District–CVRD). A discriminant analysis of CVRD residents reveals they have different views regarding tourism's potential and future in their region. A follow-up analysis, reflecting a change in the scale of enquiry and local core-periphery conditions, shows residents'perceptions and priorities will change according to their respective area groupings. This analysis reveals that residents of a peripheral region, who are expected to participate in and welcome tourism development initiatives developed by senior levels of government, will in fact have different opinions regarding the industry and its potential. These differences are linked to present levels of tourism activity within the periphery and the varying community aspirations linking tourism's development potential with local needs and priorities.     

X-ray observations of 4 Draconis: symbiotic binary or cataclysmic triple?

We present the first X-ray observations of the 4 Draconis system, consisting of an M3 III giant with a hot ultraviolet companion. It has been claimed that the companion is itself an AM Her-type binary system, an identification that places strong constraints on the evolution of cataclysmic variables. We find that the X-ray properties of 4 Draconis are consistent with the presence of an accreting white dwarf, but not consistent with the presence of an AM Her system. We conclude that 4 Draconis is therefore most likely a symbiotic binary containing a white dwarf accreting material from the wind of the red giant.
The X-ray spectrum of 4 Draconis is sometimes dominated by partially ionized photoelectric absorption, presumably due to the wind of the red giant. We note that X-ray monitoring of such systems would provide a powerful probe of the wind and mass-loss rate of the giant, and would allow a detailed test of wind accretion models.     

Simulation of Titan haze formation using a photochemical flow reactor: The optical constants of the polymer

Solar UV is the principal energy source impinging the atmosphere of Titan while the energy from the electrons in Saturn's magnetosphere is less than 0.5% of the UV light. Titan haze analogs were prepared by the photolysis of a mixture of gases that simulate the composition of its atmosphere (nitrogen, methane, hydrogen, acetylene, ethylene, and cyanoacetylene). The real (n) and imaginary (k) parts of the complex refractive index of haze analogs formed from four different gas mixtures were calculated from the spectral properties of the solid polymer in UV-visible, near infrared and infrared wavelength spectral regions. The value of n was constant at 1.6±0.1 throughout the 0.2-2.5 μm region. The variation of k with wavelength for the values derived for Titan has a lower error than the absolute values of k so the more significant comparisons are with the slopes of the k(λ) plots in the UV-VIS region. Three of the photochemical Titan haze analogs had slopes comparable to those derived for Titan from the Voyager data (Rages and Pollack, 1980, Icarus 41, 119-130; McKay and Toon, 1992, in: Proceedings of the Symposium on Titan, in: ESA SP, Vol. 338, pp. 185-190). The slopes of the k(λ) plots for haze analogs prepared by spark discharge (Khare et al., 1984, Icarus 60, 127-137) and plasma discharge (Ramirez et al., 2002, Icarus 156, 515-529) were also comparable to Titan's. These finding show that the k(λ) plots do not differentiate between different laboratory simulations of atmospheric chemistry on Titan in the UV-VIS near IR region (0.2-2.5 microns). There is a large difference between the k(λ) in the infrared between the haze analogs prepared photochemically and analogs prepared using a plasma discharges (Khare et al., 1984, Icarus 60, 127-137; Coll et al., 1999, Planet. Space Sci. 47, 1331-1340; Khare et al., 2002, Icarus 160, 172-182). The C/N ratio in the haze analog prepared by discharges is in the 2-11 range while that of the photochemical analogs is in the 18-24 range. The use of discharges and UV light for initiating the chemistry in Titan's atmosphere is discussed.