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To work with this lesson, it is important to install Tesseract OCR Engine on your system. Head over to the official Github repo to follow the installation instructions. The polarimetry of close binary systems has been modelled by Buerger & Collins II (1970) by considering the distortions on the distribution of scattering material by axial rotation and gravitational interactions The method allows calculation of intrinsic polarization in and out of eclipse Predictions are for polarization variations of several tenths of a per cent By investigating the effects of Thomson scattering in optically thin stellar envelopes, Brown, McLean & Emslie (1978) established the fundamental polarimetric behaviour associated with binary systems with co-rotating steady state electron clouds This paper is frequently cited, and the model will be referred to here as the BMcLE model The form of the variation, as plotted in the q u-plane, is dependent on the inclination, i, of the system and may be expressed in terms of the fundamental period and its rst harmonic It was demonstrated how the formulation may be formally inverted to provide a systematic diagnostic for inferring the characteristics of a binary and its envelope This seminal work has provided the basis of studies of a variety of binary types Simmons (1983) later extended the BMcLE model by considering arbitrary scattering mechanisms other than Thomson scattering, with the results illustrated by Mie scattering An alternative approach to modelling of the effects of scattering material in binary systems has been made by Dolan (1984) using regularized Monte Carlo calculations Aspin, Simmons & Brown (1981) performed an analysis of the required accuracy of q, u measurements to allow their variation to provide useful estimates of i The procedure comprised evaluation of he con dence interval of i for a model involving single Thomson scattering in a co-rotating envelope which yields an acceptable 2 t to simulated data when optimized over the free parameters involved in the model The required accuracy of polarimetric observations was found to be significantly higher for low values of inclination A later paper by Simmons, Aspin & Brown (1982) showed that tting the canonical model to binary star data will tend to yield values of inclination greater than the true value The statistical bias is most pronounced for data with higher noise values when the inferred value, and the formal linear error, have no bearing on the actual value As the noise increases, the inferred inclination approaches 90 Errors for inclination which are established by formal techniques are seriously over optimistic, except for data with high signal-tonoise ratios It was also demonstrated by Brown, Aspin, Simmons, et al (1982) that if the binary orbits are eccentric, third harmonics are generated in the polarimetric variation, making a clear diagnosis of noisy data more problematic The polarimetric behaviour of binary systems embedded in electron shells of various geometries has been explored by Manset & Bastien (2000) It was shown that the polarimetric variations should be more apparent for systems with the low inclination, a high optical depth, a at envelope, a small cavity, or an orbit that brings the stars close to the inner edge of the cavity They also demonstrated that the BMcLE model remains powerful in nding orbital inclinations & 45 for a variety of distribution forms for optically thin Thomson scattering clouds; the atness of the. ios + text recognition: Text Recognition in Vision Framework - WWDC 2019 - Videos ... java ocr tesseract githubAsprise Java OCR library offers a royalty-free API that converts images (in formats like JPEG, PNG, TIFF, PDF, etc.) into editable document formats Word, XML, ... ocr api java open source Asprise Java OCR SDK - royalty-free API library with source code ...
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The issue of whether O-type stars which, from their spectra, are known to possess variable wind structures has been taken up by Clarke, McDavid, Smith, et al (2002) For Per and Cep, analysis of a series of measurements made on single nights with individual uncertainties of p 00002, with nightly means carrying uncertainties of p 000007, suggested night-to-night variations with p 00002 It was suggested that such low-level uctuations might be engendered by structured instrumental polarization in the stellar diffraction pattern, and instrumental depolarization effects that will induce polarimetric noise according to inconsistent target acquisition and/or the action of variable seeing conditions Reassessment of the older data for Cep from Hayes (1978) also suggested that his claims for the detection of variability of this star suffer from the same problems Whether or not such supergiant stars do exhibit polarization variability requires further observational work, with careful attention being paid to the stability of repeated measurements With the advent of CCD spectropolarimetry, Harries & Howarth (1996) have investigated the H emission line of Pup (O4 I(n)f) Although data from their instrument suffered from polarizance fringes, a correction procedure was applied with the results showing that there is a polarization signature across the H emission of this star The feature is attributed to an equatorial density enhancement of the wind, their numerical model suggesting a factor of 13 for the equator-to-pole density ratio Harries (2000) has applied Monte Carlo principles to set up stellar wind radiativetransfer codes Effects of co-rotating spiral density nhancements and also effects of clumpiness within the wind were investigated Although the test runs reproduce the observed spectrometric variability of OB supergiants, the suggested polarimetric variability of these models is too weak to explain the observed behaviour of these stars A predicted spectral line polarization was noted resulting from line absorption of continuum photons in a rotating wind, the effect having a strong resemblance to the H polarimetric signal recorded by Harries & Howarth (1996) for Pup It is suggested that the recorded behaviour stems from this effect, rather than by line dilution of a continuum polarization It is of interest to note that an attempt was made by Hanbury Brown, David & Allan (1974) to measure the diameter of the supergiant Ori with orthogonal polarizations, using the Narrabri stellar intensity interferometer, in an attempt to detect any geometric distortion of the star s corona No signi cant changes of correlation were detected for the two polarizations, with no changes in the apparent diameter of the star An assessment of the possibility of success with this kind of observational technique was undertaken by Sams & Johnston (1974) using stellar models to predict the polarization It was concluded that the sensitivity would require improvements of 20 times, or more, to detect photospheric polarization in early-type stars In view of the success of other interferometric observations at H in respect of Be stars with disc structures, as described in Section 133, neglect of application of the intensity interferometer at this wavelength would seem to have missed out on making a substantial contribution here. 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