TBE is associated with morbid obesity in our population and should be considered in the differential diagnosis when evaluating mastoid and middle ear disease in the morbidly obese.

The close binary Algol system contains a radio-bright KIV subgiant star in a very close (0.062 astronomical units) and rapid (2.86 day) orbit with a main sequence B8 star. Because the rotation periods of the two stars are tidally locked to the orbital period, the rapid rotation drives a magnetic dynamo. A large body of evidence points to the existence of an extended, complex coronal magnetosphere originating at the cooler K subgiant. The detailed morphology of the subgiant's corona and its possible interaction with its companion are unknown, though theory predicts that the coronal plasma should be confined in a magnetic loop structure, as seen on the Sun. Here we report multi-epoch radio imaging of the Algol system, in which we see a large, persistent coronal loop approximately one subgiant diameter in height, whose base is straddling the subgiant and whose apex is oriented towards the B8 star. This suggests that a persistent asymmetric magnetic field structure is aligned between the two stars. The loop is larger than anticipated theoretically, but the size may be the result of a magnetic interaction between the two stars.

[1] We calculate growth rates and corresponding gains for right-hand circularly polarized extraordinary (RX) and left-hand ordinary circularly polarized (LO) mode radiation associated with the cyclotron maser instability (CMI) for parameterized horseshoe electron velocity distributions. The velocity distribution function was modeled to closely fit the electron distribution functions observed in the auroral cavity. We systematically varied the model parameters as well as the propagation direction to study the dependence of growth rates on model parameters. The growth rate depends strongly on loss cone opening angle, which must be less than 90°for significant CMI growth. The growth rate is sharply peaked for perpendicular radiation (k k = 0), with a full width at half maximum 1.7°, in good agreement with observed k-vector orientations and numerical simulations. The fractional bandwidth varied between 10 À4 and 10 À2 , depending most strongly on propagation direction. This range encompasses nearly all observed fractional auroral kilometric radiation (AKR) burst bandwidths. We find excellent agreement between the computed RX mode emergent intensities and observed AKR intensities assuming convective growth length L c % 20-40 km and group speed 0.15c. The only computed LO mode growth rates compatible observed LO mode radiation levels occurred for number densities more than 100 times the average energetic electron densities measured in auroral cavities. This implies that LO mode radiation is not produced directly by the CMI mechanism but more likely results from mode conversion of RX mode radiation. We find that perturbation of the model velocity distribution by large ion solitary waves (ion holes) can enhance the growth rate by a factor of 2-4. This will result in a gain enhancement more than 40 dB depending on the convective growth length within the structure. Similar enhancements may be caused by strong electromagnetic ion cyclotron waves.

We have used multi-epoch long-baseline radio interferometry to determine the proper motion and orbital elements of Algol and UX Arietis, two radio-bright, close binary stellar systems with distant tertiary components. For Algol, we refine the proper motion and outer orbit solutions, confirming the recent result of Zavala et al. (2010) that the inner orbit is retrograde. The radio centroid closely tracks the motion of the KIV secondary. In addition, the radio morphology varies from double-lobed at low flux level to crescent-shaped during active periods. These results are most easily interpreted as synchrotron emission from a large, co-rotating meridional loop centered on the K-star. If this is correct, it provides a radio-optical frame tie candidate with an uncertainty ±0.5 mas. For UX Arietis, we find a outer orbit solution that accounts for previous VLBI observations of an acceleration term in the proper motion fit. The outer orbit solution is also consistent with previously published radial velocity curves and speckle observations of a third body. The derived tertiary mass, 0.75 solar masses, is consistent with the K1 main-sequence star detected spectroscopically. The inner orbit solution favors radio emission from the active K0IV primary only. The radio morphology, consisting of a single, partially resolved emission region, may be associated with the persistent polar spot observed using Doppler imaging.

A survey of the literature indicates that extensive studies of the learning process with mentally retarded children have been extremely rare. The purpose of the present study was to determine the applicability of discrimination-learning methodology, originally described by Harlow (3), to the study of learning in normal and mentally retarded children. Specifically, group differences in the acquisition of an object-quality discrimination learning set were studied. Also included in this study was an empirical analysis of error factors. METHOD Apparatus and SubjectsThe testing device was the Wisconsin General Test Apparatus, slightly modified to adapt it for children (4, 5). There were 400 pairs of stimulus objects which differed from each other in multiple characteristics. These have been described elsewhere (4, 5).Subjects were eight mentally retarded children enrolled in a special opportunity class and six normal children in regular classes from the same rural elementary school. The following criteria were used in selecting the retarded group: (a) A Stanford-Binet IQ of SO to 75. A report of the child's behavior during the administration of the test was included in the analysis of the test data so that any temporary and specific conditions of the cliild at the time of testing could be given careful consideration in evaluation of the validity and reliability of the test results. (&) Comparable case history and/or psychometric data obtained in an attempt to determine the presence or absence of a relatively similar degree and type of intellectually subaverage status in one or both parents and in most siblings, (c) Available social, developmental, and academic data. These were evaluated along with psychometric results to facilitate the clinical "screening out" of those children not considered to be legitimately classified as mentally retarded, (d) Specific exclusions were epileptics, clinical types such as mongoloids, severely crippled 5s, and those with visual, auditory, or obvious neurological handicaps.The Stanford-Binct IQ range of the normal children was 90 to 109 inclusive. The means of both groups were closely matched in terms of chronological age, sex and age at which S first entered elementary school. Normal