Radiological findings of clonorchiasis

Kang, IW; Seo, H.A.; Yeon, KM

doi:10.3348/jkrs.1980.16.1.159

Cited by 4 publications

(3 citation statements)

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“…In order to explore the possible effect played by the above differences in the global efficiency of clusters to produce the CR energy flux at shocks, we applied to all simulations a recipe to estimate the CR acceleration efficiency at shocks, with a standard application of the DSA theory (e.g. Kang & Jones 2002). According to this model, the CR acceleration at each shocks is parametrized as a function of the Mach number:…”

Section: Shocks In Clusters and Cosmic Rays Accelerationmentioning

confidence: 99%

“…(v) the estimated acceleration efficiency of CR (assuming Kang & Jones 2002) is small in the innermost cluster region, f CR /f th ∼ 0.1, and increases towards the virial radius, with f CR /f th ∼ 0.8 (however, the absolute numbers are likely to change as this recipe does not account for Alfvén wave drift and dissipation at the shock precursor).…”

Section: Summary Of Shocks Propertiesmentioning

confidence: 99%

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A comparison of cosmological codes: properties of thermal gas and shock waves in large-scale structures

Vazza

Dolag

Ryu

et al. 2011

Monthly Notices of the Royal Astronomical Society

110

127

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Cosmological hydrodynamical simulations are a valuable tool for understanding the growth of large‐scale structure and the observables connected with this. Yet, comparably little attention has been given to validation studies of the properties of shocks and of the resulting thermal gas between different numerical methods – something of immediate importance as gravitational shocks are responsible for generating most of the entropy of the large‐scale structure in the Universe. Here, we present results for the statistics of thermal gas and the shock wave properties for a large volume simulated with three different cosmological numerical codes: the Eulerian total variations diminishing (TVD) code, the Eulerian piecewise parabolic method based code enzo and the Lagrangian smoothed particle hydrodynamics (SPH) code gadget. Starting from a shared set of initial conditions, we present convergence tests for a cosmological volume of side‐length 100 Mpc h−1, studying in detail the morphological and statistical properties of the thermal gas as a function of mass and spatial resolution in all codes. By applying shock‐finding methods to each code, we measure the statistics of shock waves and the related cosmic ray acceleration efficiencies, within the sample of simulations and for the results of the different approaches. We discuss the regimes of uncertainties and disagreement among codes, with a particular focus on the results at the scale of galaxy clusters. Even if the bulk of thermal and shock properties is reasonably in agreement among the three codes, yet some significant differences exist (especially between Eulerian methods and SPH). In particular, we report (a) differences of huge factors (∼10–100) in the values of average gas density, temperature, entropy, Mach number and shock thermal energy flux in the most rarefied regions of the simulations (ρ/ρcr < 1) between grid and SPH methods; (b) the hint of an entropy core inside clusters simulated in grid codes; (c) significantly different phase diagrams of shocked cells in grid codes compared to SPH and (d) sizable differences in the morphologies of accretion shocks between grid and SPH methods.

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Section: Shocks In Clusters and Cosmic Rays Accelerationmentioning

confidence: 99%

Section: Summary Of Shocks Propertiesmentioning

confidence: 99%

A comparison of cosmological codes: properties of thermal gas and shock waves in large-scale structures

Vazza

Dolag

Ryu

et al. 2011

Monthly Notices of the Royal Astronomical Society

110

127

View full text Add to dashboard Cite

show abstract

“…In numerical simulations of DSA, where the diffusionconvection equation for the evolution of the f (p) is solved in runtime, and coupled to the dynamical equation of the gas evolution (e.g. Kang & Jones 2002), the adiabatic index can be computed selfconsistently. In our case, the value of γ * cr = γ cr can only be assumed a priori.…”

Section: Spatial Advection Of Cr Energymentioning

confidence: 99%

Modelling injection and feedback of cosmic rays in grid-based cosmological simulations: effects on cluster outskirts

Vazza

Brüggen

Gheller³

et al. 2012

Monthly Notices of the Royal Astronomical Society

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We present a numerical scheme, implemented in the cosmological adaptive mesh refinement code enzo, to model the injection of cosmic ray (CR) particles at shocks, their advection and their dynamical feedback on thermal baryonic gas. We give a description of the algorithms and show their tests against analytical and idealized one‐dimensional problems. Our implementation is able to track the injection of CR energy, the spatial advection of CR energy and its feedback on the thermal gas in run‐time. This method is applied to study CR acceleration and evolution in cosmological volumes, with both fixed and variable mesh resolution. We compare the properties of galaxy clusters with and without CRs for a sample of high‐resolution clusters with different dynamical states. At variance with similar simulations based on smoothed particles hydrodynamics, we report that the inclusion of CR feedback in our method decreases the central gas density in clusters, thus reducing the X‐ray and Sunyaev–Zeldovich effect from the clusters centre, while enhancing the gas density and its related observables near the virial radius.

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Correlation of sonographic findings with histopathological changes of the bile ducts in rabbits infected with Clonorchis sinensis

Hong

Park²,

Seo³

et al. 1994

Korean J Parasitol

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Clonorchiasis is an important parasitic disease of humans in Korea. The present study intended to compare sonographic findings with histopathological changes in experimental clonorchiasis. Eighteen New Zealand white rabbits were infected with metacercariae of Clonorchis sinensis, and examined 4, 10, and 22 weeks post-infection (PI). Four infected rabbits were treated with praziquantel 10 weeks PI and were examined 12 weeks after treatment. Sonography revealed mild to severe dilatation of the intrahepatic ducts (IHDD) and slightly increased periductal echoes in 12 out of 14 rabbits at 4 weeks PI, and all of the animals after 10 and 22 weeks PI and 12 weeks after treatment. The histopathological lesions were duct dilatation, mucosal hyperplasia, and periductal fibrosis, which progressed from 4 weeks to 22 weeks PI and even in treated rabbits. The dilated intrahepatic ducts over 1 mm diameter were detected by sonography. The present results indicate that sonographic findings are well correlated with histopathological lesions in rabbit clonorchiasis except for early phase of light burden of infection. The sonography has a limitation in discriminating residual sequelae of the ducts after praziquantel treatment.

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Radiological findings of clonorchiasis

Cited by 4 publications

References 0 publications

A comparison of cosmological codes: properties of thermal gas and shock waves in large-scale structures

A comparison of cosmological codes: properties of thermal gas and shock waves in large-scale structures

Modelling injection and feedback of cosmic rays in grid-based cosmological simulations: effects on cluster outskirts

Correlation of sonographic findings with histopathological changes of the bile ducts in rabbits infected with Clonorchis sinensis

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