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For binary systems, phased-locked variations can be used to determine some of the basic orbital characteristics such as a value for the inclination, this being very important for resolving the mass function The distribution of scattering material around any system may be established with estimates for the rate of mass loss Schulte-Ladbeck (1989) discussed the importance of knowing the masses of Wolf Rayet binaries in respect of their evolution, and she emphasized the role that polarimetry plays in helping to establish a catalogue of values The appendix of her work provides a summary of 10 such systems For single stars, polarization variability provides information on asymmetries and inhomogeneities (blobs) in the stellar wind As early as 1946, Kopal & Shapley (1946) suggested that the eclipsing Wolf Rayet, V 444 Cyg, was an ideal system for investigation by polarimetry From the light curve, they concluded that the main cause of extinction in the semi-transparent envelope surrounding the WR component is scattering by free electrons, and, in turn, this would produce a small polarized ux best seen several hours before and after primary minimum Monitoring the variation of p should provide an estimate of the proportion of the light scattered, and allow determination of the longitude of the node of the binary system Early polarimetric observations of a WR star were those of McLean, Coyne, Frecker, et al (1979) using a spectral resolution of 50 , revealing that the prominent emission lines of HD 50896 = WR 6 = EZ CMa, a WN5-type star, exhibited ecreases of polarization relative to the continuum The behaviour suggested strati cation of ionization and excitation in the extended atmosphere, with the recombination lines of He II being formed deeper than those of He I, so that the ionization is decreasing outwards The continuum polarization is typical of almost pure electron scattering, suggesting that the envelope must be highly ionized and attened to some degree, or localized Later, McLean (1980) showed that the system had a polarimetric period of 1d 88, this being the second harmonic of the 3d 76 value associated with photometric and spectroscopic modulations Determination of i was made dif cult because of aperiodic instabilities, but a value of 71 was suggested, implying a 13 M companion for the 10 M primary star As a result of a photometric and polarimetric campaign, Drissen, Robert, Lamontagne, et al (1989) found that the shapes of both the light curve and the polarimetric curve changed over 2 months, but maintained the periodicity From high spectral resolution measurements, Schulte-Ladbeck, Nordsieck, Nook, et al (1990) revealed that the position angle of the polarization changed across the emission lines such that loops were executed in the q u-plane Such behaviour may be explained in terms of there being a rotating, expanding disc in the system The behaviour of the emission lines was explored further by Moffat & Piirola (1993) who found their polarization variation 03% was very much less than that of the continuum 16% For two other non-eclipsing WC7 + O binaries, they found no variation in the emission complex of C III/IV 4650 + He II 4685 , in.

Although the use of robotic sample changers has made the automation of the sample preparation and changing possible, the use of NMR tubes limits its speed and ef ciency for high-throughput applications To avoid the steps of transferring samples from a reservoir into NMR tubes and thus further increasing the throughput, an alternative solution is to use a ow NMR probe28,64 Such ow probes, which are also known as tubeless NMR probes, have a permanently mounted sample chamber or ow cell, on which an RF detection coil is usually wrapped The sample is introduced into the ow cell, and a rinsing step is necessary to eliminate the carryover from the previous sample Because the RF coil is mounted closer to the sample, an increased lling factor is obtained Therefore ow NMR probes usually have higher sensitivity than conventional NMR probes.

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contrast to the continuum modulation which provided period determinations This is perhaps to be expected in such binary systems if the orbital polarization modulation is due mainly to scattering of O-companion light off free electrons in a ot, dense, spherically symmetric WR wind; there is little or no asymmetric distribution of free electrons off which WR emission line and continuum photons can scatter and produce detectable polarization The Wolf Rayet binary system, HD 152270, has been observed by Luna (1982) and, from the phase-locked measurements, an inclination of 35 was calculated, allowing determination of the stellar masses St-Louis, Drissen, Moffat, et al (1987) presented the rst paper from the group in Montreal discussing the results of polarimetric variability in the complete sample of southern WC stars Two stars exhibited a double-wave behaviour expected of binary systems with an asymmetric distribution of scattering material within an orbiting system For HD 97152, an inclination of i D 43 5 5 was deduced, while for HD 152270, the determined value was i D 44 8 5 The WN7 binary system of HD 197406 (WR 148) was investigated polarimetrically by Drissen, Lamontagne, Moffat, et al (1986) From analysis of the oscillatory behaviour of the measurements in the q u-plane, they determined an inclination of the orbit of 67 , yielding a mass of 124 M for the unseen companion, based on a mass of 60 M for the primary, with speculation that the secondary is an X-ray quiet black hole Drissen, Moffat, Bastien, et al (1986) conducted a concentrated campaign of measurements of the WN7 binary, CQ Cep (HD 214419), which displays large polarization variations 08% They demonstrated that the second harmonic of the fundamental period was dominant, as can be appreciated by inspection of Figure 1310 Determination of the Fourier coef cients of the fundamental and second harmonic provided a value of i 78 1 , with masses of 42 M and 30 M for the WN7 star and the unseen O star companion, respectively From ve-colour measurements of CQ Cep and V444 Cyg, Piirola & Linnaluoto (1988) conclude that the polarization is generated by electron scattering in an optically thin envelope with determinations of i D 78 1 1 7, and i D 83 5 1 1, respectively Robert, Moffat, Bastien, et al (1990) have also investigated the polarimetric behaviour of V 444 Cyg and determined a value of i D 78 5, in agreement with Rudy & Kemp (1978) and Piirola & Linnaluoto (1988) Their data also showed rapid uctuations around phase 05 when the O star eclipses the scattering electrons located in the dense inner wind As well as discussing binary systems, St-Louis, Drissen, Moffat, et al (1987) described the stochastic behaviour of three single line stars The randomness of the variability of the WN8 star, HD 96548 = WR 40, is clearly portrayed in Figure 1311, there being no structure to the time progression of the measurements when plotted in the q u-plane In an immediate following paper, Drissen, St-Louis, Moffat, et al (1987) presented results of a survey of southern galactic WN stars, all of which displayed apparently random variations with amplitudes from p D 015 06% Combining these results with the data on WC stars, they found a general anti-.

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