ISO SWS Spectroscopy of WR 146 (WC6+O)

We have obtained ISO SWS spectroscopy of WR 146 (WC6+O) covering the wavelength range 2.6-20 μm. WC6 wind emission is observed in numerous lines of He II and C IV, as well as in the [Ne III] 15.5 μm line, but not in [Ne II] 12.81 or [Ne V] 14.32 μm. An analysis of these spectra (and complementary radio and optical data) yields for the WC6 star: v∞ = 2700 km s-1; M=2.6×10-5M⊙yr-1; C/He = 0.15; and a neon abundance bound of 3.4×10-3≤Ne/He≤6.8×10-3. The neon abundance is close to that predicted in stellar evolution models of WC stars. This revised version was published online in August 2006 with corrections to the Cover Date.     

Pigmenting agents in Martian soils: inferences from spectral, Mossbauer, and magnetic properties of nanophase and other iron oxides in Hawaiian palagonitic soil PN-9

We have examined a Hawaiian palagonitic tephra sample (PN-9) that has spectroscopic similarities to Martian bright regions using a number of analytical techniques, including Mossbauer and reflectance spectroscopy, X-ray diffraction, instrumental neutron activation analysis, electron probe microanalysis, transmission electron microscopy, and dithionite-citrate-bicarbonate extraction. Chemically, PN-9 has a Hawaiitic composition with alkali (and presumably silica) loss resulting from leaching by meteoric water during palagonitization; no Ce anomaly is present in the REE pattern. Mineralogically, our results show that nanophase ferric oxide (np-Ox) particles (either nanophase hematite (np-Hm) or a mixture of ferrihydrite and np-Hm) are responsible for the distinctive ferric doublet and visible-wavelength ferric absorption edge observed in Mossbauer and reflectivity spectra, respectively, for this and other spectrally similar palagonitic samples. The np-Ox particles appear to be imbedded in a hydrated aluminosilicate matrix material; no evidence was found for phyllosilicates. Other iron-bearing phases observed are titanomagnetite, which accounts for the magnetic nature of the sample; olivine; pyroxene; and glass. By analogy, np-Ox is likely the primary pigmenting agent of the bright soils and dust of Mars.     

Superstructures in ankerite and calcite

Two rhombohedral carbonates, ferroan dolomite (ankerite) and magnesian calcite from lower Jurassic ammonites, have been studied by transmission electron microscopy. The samples show small domains with the morphology of platelets parallel to (11 \(\bar 2\) 0) which have exceptionally well ordered superstructures and characteristic c-reflections. Diffraction patterns and contrast analysis of atomic resolution images indicate that the domains observed in ankerite are rich in Ca [Ca_0.75(Mg, Fe)_0.25CO₃] and those in calcite rich in Mg, and there is strong evidence that cation ordering is the cause for the observed superstructures which are proposed mainly on diffraction evidence. Rhombohedral carbonates have a close similarity to NaCl, with CO₃-groups substituting for Cl. Cation ordering patterns can therefore be discussed in analogy to f.c.c. alloys. We make use of ordering waves to describe superstructures and to qualitatively interpret kinetic conditions for their formation.     

Downstream changes of large-scale bedforms in turbidites around the Valencia channel mouth,north-west Mediterranean: implications for palaeoflow reconstruction

Side-scan sonar, seismic and core data are used to identify mega-flutes, transverse and ‘V’ shaped bedforms in turbidites around the Valencia channel mouth, north-west Mediterranean. Long-range side-scan sonar data reveal a broad, curved, asymmetric, channel, that widens and terminates downfan. The western channel bank near the channel mouth has been partly eroded by turbidity currents that spilled out of the channel. Transverse bedforms on the east of the channel floor are interpreted as antidunes and, if this interpretation is correct, they indicate that the flow was probably supercritical at least locally within the channel. Trains of mega-flutes, are incised into coarse-grained sediments of the channel floor near the channel mouth. The association of mega-flutes and antidunes is thought to be diagnostic of channel–lobe transitions on deep-sea fans. The mega-flutes pass downfan into an area of streaks that diverge at up to 45° and indicates flow expansion from the channel mouth. About 75 km downfan from the channel mouth, deep-towed side-scan data record transverse bedforms (interpreted as antidunes) passing downfan into an area covered by ‘V’ shaped bedforms with upflow pointing apices (named chevrons here). The chevrons are commonly c. 200 m from limb to limb and c. 2 m in amplitude with flow-parallel wavelengths of c. 400 m. We propose that chevrons were formed by a strong, probably supercritical (or near critical) turbidity current spreading from the channel mouth and flowing towards the Balearic Abyssal Plain. Thinning of the turbidity current, resulting from flow spreading would allow the Froude number to remain high up to 100 km from the channel mouth and could explain the observed reduction in antidune wavelength.     

Martian topography and surface properties as seen by radar: The 1971 opposition

Taking advantage of the favorable opposition of 1971, the Goldstone radar system, operating at 2388MHz, was used to scan the Martian surface. Measurements of altitude and reflected power were taken approximately every 3 days. Each measurement represents an area 8km E-W × 80km N-S, the highest resolution attained to date. Altitude measurements obtained on different observing days were combined to produce altitude profiles for three complete rotations, each at different latitudes. Large-scale variations in altitudes cover a range of 14km. Altitude changes of 5 in 30km of longitude were observed. The altitude profiles show the heavy cratering of the surface, and several large craters (50–100km) 1–2 km deep are easily seen. Reflected power for different angles of incidence was measured, yielding the scattering properties of the surface as a function of longitude. Correlation was found between the peak intensity of the reflected signal and the width of the scattering function. The average relationship between the intensity and the width suggests a power reflection coefficient of at least 0.064 ± 0.012. Departures from the average are interpreted as deviations in the reflection coefficient from the mean value. These variations are presented as a function of longitude for each of the three rotations.     

Fate and recycling of carbon compounds

This article is a brief and selective introduction to the literature and concepts concerning the fate and recycling of carbon compounds in the marine environment. It provides a framework for the other papers in the session and emphasises the areas of ignorance and the implications to be drawn from them.The fate of carbon compounds in oceanic water columns and sediments is reviewed in terms of regions and processes. Particular attention is given to certain regions — surface film and associated zone, the water column and the upper layer of the bottom sediments — and processes — microbial activity, association of organic materials and minerals and the formation and diagenesis of particulate organic matter.Most of the organic matter in the ocean is rapidly recycled but the processes, rates and fluxes are poorly understood. Major areas of ignorance include the half-lives of individual compounds and of classes of compounds and the role of microorganisms, both in the water column and in the bottom sediments. Measurements and experiments need to be conducted in the oceans and in the laboratory. Chemical and biochemical changes in the short and long term require recognition if the residual organic matter of sediments is to be interpreted in terms of past oceanic conditions.     

ISO Observations of Wolf-Rayet Dust Shells

Observations of circumstellar dust clouds of Wolf-Rayet stars made with the Short Wavelength Spectrometer on ISO reveal a subtle variety of spectral energy distributions not evident from ground-based observations. The modelling of these using the radiative transfer code "Dusty" by Ivezić, Nenkova & Elitzur is reported. The results are used to examine the contributions by different possible grain types to the emission and of circumstellar and interstellar components to the reddening. This revised version was published online in August 2006 with corrections to the Cover Date.     

Phase retrieval holography and surface adjustment of SEST using the LES-8 satellite

Phase retrieval holography has been used to determine the surface profile of the Swedish-ESO Sub-millimetre Telescope (SEST). The measurement was performed using a signal transmitted from the geosynchronous LES-8 satellite over a range of elevation angles. The results of the measurements have been used to reset the reflector thus reducing the surface errors from the initial 80 m r.m.s. to 51 m r.m.s. The improvement in the surface accuracy has been confirmed by telescope efficiency measurements at 232–250 GHz.