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free ocr api for php: free OCR processing API in PHP /jQuery/JavaScript - Stack Overflowphp ocr apiactivex ocr, perl ocr, asp.net core ocr, how to convert scanned images to searchable pdf using ocr in java, open source ocr software, handwriting ocr app android, tesseract ocr javascript, microsoft.windows.ocr c# example, ocr asp.net web application, best ocr pdf to word converter for mac, mac ocr image to text, tesseract ocr library python, vb.net ocr example, ocr software open source linux, azure cognitive services ocr pricing php ocr library tesseract - ocr -for- php / TesseractOCR . php at master ... - GitHub
A wrapper to work with Tesseract OCR inside PHP . Contribute to thiagoalessio/ tesseract - ocr -for- php development by creating an account on GitHub . pure php ocr tesseract - ocr -for- php / TesseractOCR . php at master ... - GitHub
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Get your free API key · Ordering a PRO Plan · On-Premise OCR expected net polarization, while at high inclination, the polarization is reduced by occultation Their analysis was also applied to the variation of polarization from binary systems in which the scattering material consists of a rotating onedimensional plume etween the stars, superposed on an axisymmetric disc They showed that the inclination of the system and the radial structure of the plume can be deduced for suf ciently high inclinations (i > 60 ) The extent to which the method can be generalized to an arbitrarily distributed two-dimensional scattering region was considered via Fourier analysis It was found that the inclination of the system is largely insensitive to the density distribution when the distribution function is of a simple power-law form The question was also raised that for some stars, the polar mass loss will have a greater ionization fraction than the equatorial region, such that the pole might be the dominant source for free electrons In the third paper of this series, Fox (1991) considered the effects of occultation and nite sized-source depolarization, concluding that the net polarization has a complicated inclination dependence, and that the simple result of it being p / sin2 i, obtained by Brown & McLean (1977), does not hold For Be stars with high intrinsic polarizations, the circumstellar envelope must be concentrated either towards equatorial or polar regions, and that a substantial optical depth is required with > 005 The possible variability of the observed polarization from an obliquely rotating envelope has been investigated by Fox (1992), such a scenario having been mooted by others as being an alternative interpretation to diagnoses involving binary motion, but with lack of spectroscopic evidence to add weight to such duplicity The results of the exercise were not too sanguine as it was evident that effects due to rotation about a body axis and binary orbital motion are indistinguishable It was also found that the physical geometry of the obliquely rotating envelope could not be inferred When the light source is considered to have nite extent, discrimination between envelope geometries emerges to some degree as a result of the occultation of parts of the envelope by the extended source Further modelling by Fox (1993a) has emphasized the effect that an extended light source has on the resulting polarization by scattering in circumstellar envelopes If the underlying star is non-spherical, as a result of its large rotational velocity say, its photosphere will also generate a net polarization, adding to that which is produced by scattering within the extended atmosphere This situation has been modelled by Fox (1993a) who found that, in general, the predicted polarization was a factor of 2 3 times larger than what is observed for Be star systems It was also noted that the theoretical models for Be star envelopes had not yet reached a level of sophistication to estimate by polarimetry the number density of free electrons throughout the circumstellar envelope The origin of stellar winds in Be stars may be in uenced by magnetic elds and Fox (1993b) has considered this additional parameter in polarimetric models From his analysis, the range of observed values of p can be explained if the stars possess small magnetic elds of B0 < 100 G Observed increases in p during the onset of a shell phase is indicative of an increased magnetic eld. perl ocr: Tesseract (software) - Wikipedia php ocr library Getting started with Optical Character Recognition ( OCR ) with ...
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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 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. 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