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Our thoughts arise from coordinated patterns of interactions between brain structures that change with our ongoing experiences. High-order dynamic correlations in neural activity patterns reflect different subgraphs of the brain’s functional connectome that display homologous lower-level dynamic correlations. Here we test the hypothesis that high-level cognition is reflected in high-order dynamic correlations in brain activity patterns. We develop an approach to estimating high-order dynamic correlations in timeseries data, and we apply the approach to neuroimaging data collected as human participants either listen to a ten-minute story or listen to a temporally scrambled version of the story. We train across-participant pattern classifiers to decode (in held-out data) when in the session each neural activity snapshot was collected. We find that classifiers trained to decode from high-order dynamic correlations yield the best performance on data collected as participants listened to the (unscrambled) story. By contrast, classifiers trained to decode data from scrambled versions of the story yielded the best performance when they were trained using first-order dynamic correlations or non-correlational activity patterns. We suggest that as our thoughts become more complex, they are reflected in higher-order patterns of dynamic network interactions throughout the brain., Coordinated patterns of brain activity reflect cognitive processes. Here the authors use a mathematical framework for describing dynamic patterns in brain networks to show they organize in a fractal-like hierarchy during story listening.

This repository contains data and code used to produce the paper High-level cognition during story listening is reflected in high-order dynamic correlations in neural activity patterns by Lucy L.W. Owen, Thomas H. Chang, and Jeremy R. Manning. You may also be interested in our timecorr Python toolbox for calculating high-order dynamic correlations in timeseries data; the methods implemented in our timecorr toolbox feature prominently in our paper.

Abell 30 is the brighter of only two planetary nebulae that show extended X-ray emission. Our recent ROSAT high-resolution imager observation of A30 reveals a central source at a 4 σ level and emission knots at a 2 σ level. These emission features are within the same region as the H-deficient knots and filaments resolved in a previous HST WFPC2 [O III] image. The ROSAT position of the X-ray peak is offset by 28 from the HST position of the central star of A30. Since the ROSAT pointing may be uncertain by up to 10'', we assume that the X-ray peak is aligned with the central star. The two brighter X-ray emission knots then become aligned with prominent [O III] features in the nebula. Ground-based echelle observations and HST WFPC2 images of A30 reveal a bipolar pair of knots and a clumpy expanding disk. The morphology and velocity structure of the bipolar knots and disk show evidence of the stellar wind ablating the knots and clumps. An efficient mixing of the shocked stellar wind and the ablated material is needed to produce the low plasma temperature, 4.5 × 105 K, and the high electron density, ~1000 cm-3, derived from the observed X-ray flux and spectral distribution.

We have measured the analyzing power for elastic scattering of {pi}{sup +} from a target of polarized {sup 1}H. Data were taken for incident pion beam energies of 165 and 240 MeV at several pion scattering angles. The current data generally agree with previously existing measurements of {ital A}{sub {ital y}} for this reaction and also with results of the SAID phase-shift analysis program. In most cases the new data are of higher precision than previously existing data. {copyright} {ital 1996 The American Physical Society.}

This report describes the cases of two patients who underwent laparoscopic repair for treatment of Morgagni-Larrey hernia at United Hospital Center in Clarksburg. The first patient was a 40-year-old woman complaining of epigastric discomfort and tenderness. Her chest X-ray revealed an anterior cardiophrenic mass, and a CT scan showed a characteristic Morgagni hernia with incarcerated colon and omentum. After reduction of the incarcerated bowel and omentum, autosuture repair was carried out laparoscopically In the second case, a 22-year-old man with severe GERD was found to have a large Morgagni hernia with incarcerated transverse colon and omentum, which was discovered while he was undergoing an elective laparoscopic Nissen fundoplication. Laparoscopic repair of Morgagni hernia was carried out, in addition to Nissen fundoplication. Both patients did very well postoperatively. Minimally invasive laparoscopic repair can be successfully carried out, and mesh implantation is performed only in some cases. In order to avoid pleural injury, we prefer not to remove the hernia sac before a Morgagni hernia is repaired. Laparoscopic repair should be considered the standard and safest procedure for the treatment of a Morgagni hernia.

The large H II complex N11 in the Large Magellanic Cloud contains OB associations at several different stages in their life histories. We have obtained ROSAT PSPC and HRI X-ray observations, Curtis Schmidt CCD images, echelle spectra in H-alpha and [N II] lines, and IUE interstellar absorption line observations of this region. The central bubble of N11 has an X-ray luminosity a factor of only 3-7 brighter than predicted for an energy-conserving superbubble, making this the first detection of X-ray emission from a superbubble without a strong X-ray excess. The region N11B contains an extremely young OB association analogous to the central association of the Carina nebula, apparently still embedded in its natal molecular cloud. We find that N11B emits diffuse X-ray emission, probably powered by stellar winds. Finally, we compare the tight cluster HD32228 in N11 to R136 in 30 Dor. The latter is a strong X-ray source, while the former is not detected, showing that strong X-ray emission from compact objects is not a universal property of such tight clusters., submitted to ApJ 1 April 1997, uses aasms4.sty, 20 pages, 10 figures (figure 3 is color; figures 1a and 4 are gifs; original postscript available from http://www.mpia-hd.mpg.de/MPIA/Projects/THEORY/maclow/papers/n11/n11.html