Received; accepted – 2 – We have searched 101 Classical transneptunian objects for companions with the Hubble Space Telescope. Of these, at least 21 are binary. The heliocentric inclinations of the objects we observed range from 0.6-34 ◦. We find a very strong anticorrelation of binaries

Abstract. Colours distributions have been studied in 12 S0 galaxies, most of these nearly edge-on, from high reso-lution frames obtained at the CFHT and the Pic du Midi 2 m telescope, supplemented for some purposes by low res-olution frames from the Observatoire de Haute Provence 120 cm telescope. Great attention has been given to reduce the eects of \dierential seeing", resulting from dierent PSF’s in the two frames needed for a colour measurement. Errors from various sources, and their eect upon measured quanti-ties, have been evaluated from the study of pseudo-colours (obtained by applying our measuring techniques to pair of frames taken in the same passband), and from the com-parison of colours data from our various series. Data are given about the following topics: { Radial isophotal colour proles, leading to reference colours at re and gradients in 4 colour indices (except for missing data); { Reference colours and gradients in possibly dustless re-gions of nearly pure bulge or disk, allowing a comparison between the two components; { Dust patterns, seen in 7 objects; { Systematic dierences between major and minor axis colours upon isophotal contours (outside dust patterns). Both a redder or bluer major axis are encountered de-pending upon the object, or the central distance in a given object. The observations may sometimes be explained by local dust concentration in disks. In other cases popula-tion dierences between spheroidal and disk components should be invoked; { Asymmetries in light and colour distributions along the minor axis in 3 objects, due to dust concentrated in the disk; Send oprint requests to: R. Michard? Based on observations collected at the Canada-France-Hawaii Telescope, the Observatoire du Pic du Midi and the Observatoire de Haute-Provence. { Correlations between ring structure and major axis colour proles.

on the rela-tive size of the bubble and channel height and less strongly dependent on inclination angle and coefficients of viscosity and surface ten-sion. NOMENCLATURE A Bubble cross sectional area C Volume fraction of phase 1 g ̂ Gravity unit vector

be relatively automatically evoked in response to an oVense. Four studies provide evidence relevant to this general hypothesis. Studies 1 and 2 demonstrate that the subliminal presentation of close others (versus non-close others or a control word) induces a relatively strong inclination to forgive various o

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an upper region of strong chemical stratification. This gradient region increases in depth with time and is separated by a sharp interface from a region of homogeneous solution below. Eventually the whole depth of fluid becomes chemically stratified. When crystallization occurs along an inclined floor thin

Abstract. In this paper we prove that if a mapping µ from incline R into [0, 1] is a fuzzy homomorphism then the incline order relation is preserved and the crisp sets that is, complement of strong α-cuts are ideals of R. We provide sufficient conditions for µ to be a fuzzy homomorphism. Further we

. This study examined the three-dimensional whole-body angular momentum patterns of 30 healthy subjects walking over a range of incline and decline angles. The range of angular momentum was either similar or reduced on decline surfaces and increased on incline surfaces relative to level ground

Abstract—In this work, new experimental data for slugging frequency in inclined gas-liquid flow are reported, and a new correlation is proposed. Scale experiments were carried out using a mixture of air and water in a 6 m long pipe. Two different pipe diameters were used, namely, 38 and 67 mm

reported here suggest that a third optical mechanism influences the OE: some parts of the mud polygon are more strongly illuminated than others, depending on the angle of incidence of sunlight. This causes the areas facing the observer and the sun to be brighter than the rest of the polygon field