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Fig 136 Two mass loss events are displayed for Ori showing a rapid rise of the recorded polarization followed by a slow decay (The JD is 2 440 000C) (Data taken from Hayes & Guinan, 1984 and Sonneborn, Grady, Chi-Chao Wu, et al, 1988)
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haviour was ascribed to effects of mass loss, but with the scattering material preserving axial symmetry Over a monitored mass loss episode, they found a strong correlation between the variations of continuum photometry and polarimetry, with H line photometry also being correlated, but to a lesser extent The increase in envelope mass during the event was estimated to be > 6 10 11 M A further mass loss episode was monitored by B-band polarimetry, but with a more comprehensive diagnosis by Sonneborn, Grady, Chi-Chao Wu, et al (1988) involving inclusion of other multi-parameter observational material Variations in visual colours and continuum uxes were correlated with p The lack of correlation between the highly ionized stellar wind, as observed in IUE spectra, and the continuum polarization and ux variations, was interpreted as evidence for the spatial separation of the wind-accelerated zone and the inner portion of the envelope Similarly, the lack of correlation between the H uxes and continuum changes was interpreted as indicating that the H line-formation zone is much more extended than the regions of the envelope where the stellar wind lines and the polarization are formed A straightforward interpretation of the available data is that the continuum polarization, continuum-magnitude changes, and colour changes are produced in an equatorial disc close to the stellar photosphere In an exercise to relate the variable optical polarization and UV narrow absorption lines in Be stars, Brown & Henrichs (1987) considered the data for Ori It was concluded that there are two types of mass loss occurring One involves ap-
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Fig 137 B-band polarization measurements of Ori over the interval Sep 9, 1981 to Nov 10, 1982 follow a path along an intrinsic line, indicating that the underlying mass loss event has maintained axial symmetry The dashed line denotes the interstellar polarization deduced from eld stars (Taken from Hayes & Guinan, 1984)
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proximately spherical shell enhancements of the normal wind, these lasting 20 days and are responsible for narrow UV line transients, but are not suf ciently dense, or aspherical, to give polarimetric signals The second is in the form of episodic mass ejections lasting & 40 days, affecting the global distribution of the circumstellar disc material The polarization grows along the intrinsic line, the direction corresponding to the projection of the stellar equator; both optical and H photometry display correlated changes with p Closer inspection of the u values, as they scatter about the intrinsic line suggest an oscillatory behaviour as the polarization grows and declines along the intrinsic q direction A period search on the intrinsic u values by the author was inconclusive in relation to the photometric period of 0d 99, or double light-curve of 0d 525, discovered by Balona, Marang, Monderen, et al (1987), as the polarization behaviour was sampled with too large a time interval It would be pro table to conduct polarimetry in a concentrated way
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over a number of consecutive nights A careful study of the data behaviour possibly indicates that the decay around JD 5000C has intrinsic u values providing a local mean that is not zero; the effect can be seen in the mid section of the plot in Figure 137 where the data points tend to lie on the left of the intrinsic line This would indicate that the dispersal of the ejected material is not exactly axisymmetric The Be star, X Per = HD 24534, became of particular interest when it was proposed to correspond to the X-ray source 3U 0352 + 30 An extensive observational programme was undertaken by Kemp & Barbour (1983) who obtained 400 measurements on 356 nights during 1977 1982 According to their analysis, part of the polarimetric variability was correlated with a then promoted 580d radial velocity cycle Later, Clarke & McGale (1988) reworked the data with a variety of reduction methods, and promoted the presence of a very signi cant and much shorter period of 23h 95 0h 95, commenting that X Per behaves as an oblique rotator with i D 50 10 , with the scattering source located at high stellar latitude This short period occurs in the periodogram of Kemp & Barbour (1983), but is not clearly presented, being located at a break in the sectioned graph Such a period is, of course, awkwardly close to values that can be arti cially generated by taking nightly measurements, but care was taken in assessing this potential problem Possible polarizational changes across H and H were investigated by Clarke & McLean (1975) with a null result As part of an exercise to measure the polarization of 14 Be stars, Lin & Zihe (1988) made special comment on 8 of them which had been observed on 6 or more nights It was claimed that all of them exhibited temporal changes, but without any intrinsic lines being obvious For CX Dra, when the Stokes parameters were phased on a period which is half the known orbital period of this binary system, both q and u presented a clear oscillation Annual monitoring of the long-term temporal behaviour of a number of brighter Be stars has been conducted by McDavid (1986, 1990, 1994), his work covering an interval of 9 years No strong cases of night-to-night variability were discovered, and only Aqr displayed signi cant long term variations, with a comment that these could be readily explained by changes in the circumstellar electron number density
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