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The special clinical value of Object Assembly, according to Wechsler, therefore derives from the examiner s opportunity to observe firsthand the subject s mode of perception, the degree to which he relies on trial and error ethods, and his manner of reaction to mistakes (1958, p. 84). Digit Symbol-Coding The Digit Symbol or Substitution Test is one of the oldest and best established of all psychological tests. It is to be found in a large variety of intelligence scales, and its wide popularity is fully merited (Wechsler, 1958, p. 81). The W-B I Digit Symbol subtest was taken from the Army Beta, the only change being the reduction in response time from 2 minutes to 1 1 2 minutes to avoid a pileup of perfect scores. For the WAIS, the number of symbols to be copied was increased by about one third, although the response time remained unchanged. Wechsler s (1958) main concern regarding the use of Digit Symbol for assessing adult intelligence involved its potential dependency on visual acuity, motor coordination, and speed. He discounted the first two variables, except for people with specific visual or motor disabilities, but gave much consideration to the impact of speed on test performance. He was well aware that Digit Symbol performance drops dramatically with increasing age and is especially deficient for older individuals, who do not write or handle objects as fast as younger persons, and what is perhaps equally important, they are not as easily motivated to do so. The problem, how-. size, image with .net barcode sdk. Barcode encoder for .net . data matrix data, size, image with vb barcode sdk. .Related: 



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There was also a spike-like excursion across the blue-shifted absorption feature, the position of this matching the orientation of a highly inclined disc recorded as a long-wavelength image by other observers As part of a spectroscopic campaign of observations of HD 163296 (Herbig Ae), Beskrovnaya, Pogodin, Yudin, et al (1998) reported on Q, U, V polarimetry over a 13 night run The nightly means for the U parameter for each of three colours (VRI) revealed steady night-to-night increases, but superimposed on this trend, a sinusoidal oscillation with amplitude 01%, and a period of P D 7d 5 0d 3, was noted The variations in the Q parameter were less distinct, but could also be tted by a sinusoidal curve with the same period, and shifted in phase by /4 relative the variation of U Low levels of circular polarization (V parameter) were claimed seemingly to increase across the spectrum from the B-band to the I-band Variations of the nightly means were correlated with those of p These results implied the presence of aligned particles in the circumstellar environment Beskrovnaya, Pogodin, Miroshnichenko, et al (1999) have also undertaken a multi-parameter study of he Herbig Ae candidate, HD 36112, including polarimetry As with other classical Herbig Ae stars, long-term trends and more rapid changes during a single night were recorded The variations are in accord with the hypothesis of orbital motion of different circumstellar inhomogeneities rotating in the common attened gaseous-dusty envelope A two-colour study by Clarke, Smith & Yudin (1999) of the Herbig Be star, HD 100546, showed polarimetric variability that was likely caused by changes in the distribution of dust within the stellar environment The young Herbig Ae star, HD 139614, has also been shown to be a polarimetric variable by Yudin, Clarke & Smith (1999) and, in the same paper, comments are made on the differences of polarimetric behaviour of Vega-type stars Photopolarimetric activity of the classical Ae/Be star RR Tau has been discussed by Rostopchina, Grinin, Okazaki, et al (1997) This star has a photometric variability of 4m in the V-band The value of p anti-correlates with brightness changes In addition, colour magnitude diagrams display a strange behaviour with the colour index having the same values at maximum and minimum light, this being referred to as the turnaround effect The overall behaviour of RR Tau is classical with respect to a set of young stars exhibiting non-periodic Algol-type minima, UX Ori being the prototype, giving rise to a category of stars referred to as UXORs The behaviour of p is predicted in the framework of a variable circumstellar extinction model, and is a result of the screening of the young star by opaque fragments, or clouds, in the protoplanetary disc (Grinin s model) After estimating the interstellar component for RR Tau, numerical modelling of the intrinsic polarization together with the colour magnitude diagrams indicates that the revolving circumstellar disc around this star is strongly attened, and seen edge on, or under small inclination to the line of sight The characteristic size of the grains are intermediate between that of interstellar dust and dust in the old protoplantery disc It is thought to be a young progenitor of a Pictoris-type star The disc of this latter star has been imaged with polarization vector maps by Gledhill, Scarrott & Wolstencroft (1991) and Wolstencroft, Scarrott & Gledhill (1995) Modelling of the dust disc has been undertaken.





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by Voshchinnikov & Kr gel (1999), with the result that grains have refractive index in the R-band of m R D 1152 0005i, with size distribution expressed by n(a) a 32 , the decreasing number density with distance from the star being expressed by r 3 Oudmaijer & Drew (1999) have presented data of the polarization structures across the H emission lines in several B[e] and Herbig Be stars All the B[e] stars showed large changes of p, across the H emission features, whereas only about half the Herbig Be objects displayed polarization changes A comprehensive analysis of the correlations between the polarimetric and photometric characteristics of Ae/Be stars has been made by Yudin (2000) There is a general relationship between the optical polarization and the infrared colour index (V L)obs , and the colour excess, E(V L) , as a result of circumstellar dust shells Most young stars have statistically larger values of p in comparison with stars which are at an evolutionary stage prior to their arrival at the main sequence The notion that the polarimetric behaviours of young stars relate to the evolution of their circumstellar shells has been strongly promoted Polarimetric changes across H are generally very evident in Herbig Ae/Be stars, as reported in an observational study of a sample of 23 objects by Vink, Drew, Harries, et al (2002) From their observations, they note that the signatures for Ae stars differ from Be objects, with depolarization across H in Be stars, and with polarization enhancements in the Ae group It has been suggested that the differences in behaviour may be an indication that there is a transition in the HR diagram from magnetic accretion at spectral type A, to disc accretion at spectral type B Alternatively the interior polarized line emission apparent in Ae stars may be masked in Herbig Be stars, owing to their higher levels of H emission A search for the presence of magnetic elds in three Ae stars was made by Hubrig, Sch ller & Yudin (2004) using circular polarization line wing measurements A longitudinal eld of 450 93 G was measured for HD 139614, and suspected eld detections were reported for HD 144432 and HD 144668 For the latter two stars, circular polarization signatures were noted in the Ca II K line.

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