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for all the Miras Little or no line effects were noted for R Sct An example of these data is presented in Figure 142 for R And Using narrow-band lters to isolate strong features such as the TiO bands and the CaI line at 4226 , Codina-Landaberry & Magalh es (1980) have observed four Miras in the Southern Hemisphere, and the semi-irregular variable L2 Pup ariability was found in the TiO bands in all of the target stars The behaviour is thought to be controlled by the variation of the source function, and the ratio of absorption to scattering, as a function of optical depth in the stellar photosphere For L2 Pup, there were polarization changes across the calcium line, indicating that CaI is unevenly distributed across a stellar surface Further narrow-band measurements were made of L2 Puppis by Magalh es, Coyne, Codina-Landaberry, et al (1986) over a 3-year period Systematic changes were recorded in both p and , being most noteworthy for the CaI 4226 atomic line The behaviour was best explained by a combination of photospheric effects including a non-uniform distribution of Ca across the stellar disc, and scattering from dust grains in an asymmetric cloud about the star, in which there is a systematic time variation in grain size with distance from the star A sample of Mira-type variables was monitored by Boyle, Aspin, Coyne, et al (1986) with 20 resolution over the blue end of the spectrum The most remarkable feature of the study was the behaviour of the resonance line, CaI 4226 Many of the surveyed stars, but not all, showed enhanced p in this atomic line, with several revealing rotation of the direction of vibration relative to measurements of the nearby continuum For some stars, there is a decrease in p across the TiO bands, whereas for others there is an increase It is argued that these behavioural features require more than one polarigenic mechanism, and that both photospheric and circumstellar processes are important Spectropolarimetric studies have been made by Bieging, Schmidt, Smith, et al (2006) for a selection of asymptotic giant branch (AGB) and post-asymptotic giant branch stars Most of the objects exhibited intrinsic polarization with features being detectable in the various molecular lines Effects were recorded in the TiO bands of three M-type Mira variables, in the CN bands of the carbon stars R Lep and V 384 Per, and in the Swan bands of C2 in R CrB and two proto-planetary nebulae Polarization effects in the molecular bands appear to be more common, and the effects are larger, in O-rich rather than C-rich objects.

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The tags in this taxonomy would only be used by the theme, by adding classes to the post div or perhaps the body tag here s no default support for this, but it can be used nonetheless by adding it to the theme using a few snippets of code You can also imagine some taxonomies overlapping with custom fields, since some usage of this feature is all about sorting posts Taxonomies are better suited for this by nature It is, however, when larger amounts of content need to be controlled that taxonomies reach their full potential Taxonomies are, after all, a sorting feature and that means they work best when there is actually something to sort At first it can be a bit daunting to wrap your mind around the possibilities that custom taxonomies offer.

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This freedom can be put to good use, and with the ease of adding new taxonomies that comes with WordPress 28, I m sure there will be several WordPress-powered sites putting taxonomies to useful work soon You, as an end user, may not see it, but the developer may not have to write a bunch of plugins or strain the not so user-friendly custom fields to achieve the content sorting and presentation needed So don t forget about taxonomies just because the documentation on them is limited and it isn t a function that is widely used yet; it is still a feature to be considered Sometimes you just need one place to provide the necessary data to make the site behave like you want it to.

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or ( ), was seen across this intense feature and the general form of p ( ) corresponded to the behaviour expected of Serkowski s Law It was concluded that the recorded polarization was clearly interstellar Intrinsic circular polarization, however, was detected with a Zeeman-like structure across the H emission The estimated eld in the emission region was 100 G If the system is interpreted as being a pair of dwarf stars, this implies an impossibly large eld, 1017 G, at the nucleus, say at the white dwarf surface The situation is reconcilable by considering the outburst to be highly asymmetrical, taking the form of conical and polar plumes such that geometry requires very high, but reasonable, elds on the surface of the central star This scenario was revealed more dramatically by Stockman, Schmidt & Lamb (1988) when the same nova had declined by late 1987 to magnitude 17 and relabelled as V 1500 Cygni Circular polarization was detected and interpreted as high harmonic optical cyclotron emission from an accreting, magnetic white dwarf primary They recorded a periodic variation of v at P D 0d 137154, with a semi-amplitude of 15%, corresponding to the rotation period of a star with a large dipolar eld The suggestion is that the pre-nova system was a synchronised AM Her magnetic variable During the outburst and subsequent dense wind phase, coupling between the white dwarf and expanded envelope produced the change in period rst noted by photometry Substantial polarization variation during minimum light at the eclipse stage of DQ Her was monitored by Dibai & Shakhovskoi (1967), thus allowing determination of the position for the orbital plane of the close binary system, this being very similar to the direction of the major axis of the envelope after the 1934 nova outburst Perhaps the most remarkable polarimetric discovery related to the same object displaying a remarkable 71-second light variation, is that of Swedlund, Kemp & Wolstencroft (1974) who found variable circular polarization ith a period of 142 s, or twice that of the light period It was concluded that the object contains an oblique magnetic rotator The same research group (Kemp, Swedlund & Wolstencroft, 1974) also discovered a periodic linear polarization with the same period of 142 s, and offered a simple model The nova-like system V 3885 Sgr, sometimes referred to as Bond s star, was observed in 1983 by Metz (1989) to investigate the binary character of the system The standard deviations of the measurements were surprisingly in accordance with photon statistics, with no periodicity detectable Phase diagrams were constructed around various assumed values, but no periodic variation was signi cant, with the conclusion that the study of polarization does not help the understanding of this object Nova Cassiopeiae 1993, or V 705 Cas was monitored by Okazaki, Kurihara, Hirata, et al (1996) in its early stages and was found to display irregular variations of p on time scales of several days, and it was suggested that its intrinsic polarization in the early decline phase was caused by dust scattering The observations were modelled by Kawabata, Seki, Matsumuru et al (1996) who suggested that that the dust size distribution was quite narrow in the early stages of the outburst, but became wider later.

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