Stellar P larimetry in .NET

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over an interval of 500 , with a fairly at behaviour from thereon to 8500 Again, the structures in the p ( ), ( ) records require a combination of two or more polarigenic mechanisms, with the detailed variations in the molecular absorption bands explained by the existence of photospheric hotspots (convection cells) on the cool stellar component of the system Later, Schwarz & Aspin (1987) noted that both p and displayed large temporal variations with a change of 1% to 10% in the Uband The signi cant p dip at the OIII emission line, previously noticed in earlier data, is also commented on as being subject to dramatic changes according to the Mira phase of this object The value of p was found to have a maximum at minimum light, the sense of the correlation being opposite to that of o Ceti, as reported by Shawl (1974) A very remarkable discovery was made related to the 6825 and 7082 emission features in the spectra of symbiotic stars when they were diagnosed by Schmid (1989) as resulting from a Raman scattering process This involves the absorption of radiation at some wavelength with re-emission at another The process of remission is dipole in nature, and consequently the redirected energy is likely to exhibit polarization The concepts of the scenario have been brie y described by Schild & Schmid (1992) A simple geometric model, which allowed its exploration by Monte Carlo simulations, was presented by Schmid (1992) The basic model suggests that the variation of p may be simply expressed as p D p max sin2 , (141)
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where is the angle between the line of sight and the binary axis connecting the two stars This in turn may be expressed as p D p max cos2 ' cos2 i C sin2 ' , (142)
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with the orbital phase, ', being given by the photometric phase The temporal variations of the polarization signatures of the Raman lines at 6825 and 7082 thus provide unique information on the geometry of the orbit such as the inclination, i, the orientation of the line of nodes, , and the sense of its description The geometry requires strong O VI radiation produced in the ionized region near the hot component, and converted by neutral hydrogen into Raman photons in the extended atmosphere and wind of the cool giant As the binary orbit is executed, the scattering geometry rotates relative to the line of sight A phase-locked rotation of the position angle, , is expected For an orbit with inclination, the rotation of is faster near conjunction and slower nearer quadrature The values of p are expected to be at a minimum near conjunction, being closest to a forward or backward scattering situation; higher values of p will occur at the quadratures which offer scattering nearer to 90 In addition, information on the geometric structure of the nebular O VI region, and on absorbing particles in the outer atmosphere of the red giant, may be obtained The orientation of the orbital plane can be determined from measurements of , particularly in the blue wing of the Raman lines The reason for this is that these photons originate predominantly from scattering close to the binary axis where
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14 Late-type Stars
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the neutral hydrogen atoms in the giant s wind move towards the O VI source, introducing a blueward Doppler shift The red wing emission originates from the receding (relative to the O VI source) outer part of the giant wind, which is geometrically less de ned, and where geometric cancellation of the polarimetric signal is important Thus, the orientation of the line of nodes may be determined from measured at the orbital quadrature phase Based on such a scenario, monitoring of the Raman lines allows determinations of orbital parameters such as period, inclination and orientation of the orbital plane In addition, information on the geometric structure of the nebular O VI region and on absorbing particles in the outer atmosphere of the red giant may be obtained As a result of a survey of 15 symbiotic stars, Schmid & Schild (1994) found high values of p across the noted Raman lines with effects integrated over the emission pro les of about 5% Three types of structure seem to present themselves: I Pro les with constant p across the lines II Pro les with decreasing p towards the red line wing and constant direction of vibration III Pro les with two components and a rotating or ipping vibration angle The morphological differences in the pro le polarization structures can be accounted for by the simple geometric model Spectropolarimetric observations were made by Schild & Schmid (1996) of the symbiotic Mira, V 1016 Cygni, covering the broad emission features at 6825 and 7082 A data record is depicted in Figure 144 showing these features in emission, with q and u signatures on an otherwise at polarimetric continuum They found that p increased over a 3-year interval, and that the azimuth of the polarization in the blue wing of the lines rotates clockwise at a constant rate of 8 2 per year From these data, it was concluded the binary system has a period of 80 25 years and that the orbit inclination is 60 20 In August 1991, the binary axis projected on the celestial sphere was at position angle 81 , but had rotated to 58
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Fig 144 In the upper section, spectral records of V 1016 Cygni in Sep 1994 reveal the strong emission features at 6825 and 7082 The lower records for q and u indicate that the same two emissions are the only features carrying a polarimetric signature (Taken from Schild & Schmid, 1996)
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