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IRIS Mobile OCR SDK enables developers to easily integrate imaging features and OCR capabilities into their mobile applications. ... IRIS mobile OCR Software development kit allows developers to create custom mobile imaging applications to convert all pictures and images into indexed ... 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 enhancements 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 ffect 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. leadtools ocr sdk free download: Epson Document Capture Suite for scanners - Epson ocr sdk for mobile C# OCR SDK for High Performance OCR and OCR PDF Applications
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