To the Detection of Bondline Flaws in Rubber/Metal Laminates a Comparison of the Sensitivity of Transverse and Lamb Waves

The use of adhesively-bonded structures is prevalent throughout the Navy since watertight rubber-to-metal bonds are required on many undersea systems including sonar transducers and electrical cables. In addition, adhesive bonds are used to transfer loads between rubber and metal adherends for limited structural applications. However, in each case the principal function of the adhesive bond is to provide watertight integrity for the bonded components in the hostile ocean environment where corrosion is of major concern

Solid State Neutral Particle Analyzer Array on NSTX

A Solid State Neutral Particle Analyzer (SSNPA) array has been installed on the National Spherical Torus Experiment (NSTX). The array consists of four chords viewing through a common vacuum flange. The tangency radii of the viewing chords are 60, 90, 100, and 120 cm. They view across the three co-injection neutral beam lines (deuterium, 80 keV (typ.) with tangency radii 48.7, 59.2, and 69.4 cm) on NSTX and detect co-going energetic ions. A silicon photodiode used was calibrated by using a mono-energetic deuteron beam source. Deuterons with energy above 40 keV can be detected with the present setup. The degradation of the performance was also investigated. Lead shots and epoxy are used for neutron shielding to reduce handling any hazardous heavy metal. This method also enables us to make an arbitrary shape to be fit into the complex flight tube

6.7 GHz methanol absorption toward the Seyfert 2 galaxy NGC 3079

The detection of the 6.7 GHz line of methanol (CH3OH) is reported for the first time toward an object beyond the Magellanic Clouds. Using the Effelsberg 100 m telescope, two absorption features were identified toward the Seyfert 2 galaxy NGC 3079. Both components probably originated on lines-of-sight toward the central region, presumably absorbing the radio continuum of the nuclear sources A, B, and E of NGC 3079. One absorption feature, at the systemic velocity, is narrow and may arise from gas not related to the nuclear environment of the galaxy. The weaker blue-shifted component is wider and may trace outflowing gas. Total A-type CH3OH column densities are estimated to be between a few times 10^13 and a few times 10^15 cm^-2. Because of a highly frequency-dependent continuum background, the overall similarity of HI, OH, and CH3OH absorption profiles hints at molecular clouds that cover the entire area occupied by the nuclear radio continuum sources ~ 4 pc.Comment: 4 pages, 1 figure, accepted for publication in A&A Letter

Chandra Observations and the Nature of the Anomalous Arms of NGC 4258 (M 106)

This paper presents high resolution X-ray observations with Chandra of NGC 4258 and infers the nature of the so called ``anomalous arms'' in this galaxy. The anomalous arms dominate the X-ray image; diffuse X-ray emission from the ``plateaux'' regions, seen in radio and H$\alpha$ imaging, is also found. X-ray spectra have been obtained at various locations along the anomalous arms and are well described by thermal (mekal) models with kT in the range 0.37 - 0.6 keV. The previously known kpc-scale radio jets are surrounded by cocoons of hot X-ray emitting gas for the first 350 pc of their length. The radio jets, seen in previous VLBA and VLA observations, propagate perpendicular to the compact nuclear gas disk (imaged in water vapor maser emission). The angle between the jets and the rotation axis of the galactic disk is 60$^{\circ}$. The jets shock the normal interstellar gas along the first 350 pc of their length, causing the hot, X-ray emitting cocoons noted above. At a height of z = 175 pc from the disk plane, the jets exit the normal gas disk and then propagate though the low density halo until they reach ``hot spots'' (at 870 pc and 1.7 kpc from the nucleus), which are seen in radio, optical line and X-ray emission. These jets must drive mass motions into the low density halo gas. This high velocity halo gas impacts on the dense galactic gas disk and shock heats it along and around a ``line of damage'', which is the projection of the jets onto the galactic gas disk as viewed down the galaxy disk rotation axis. However, because NGC 4258 is highly inclined ($i$ = 64$^{\circ}$), the ``line of damage'' projects on the sky in a different direction to the jets themselves. We calculate the expected p.a. of the ``line of damage'' on the sky and find that it coincides with the anomalous arms to within 2$^{\circ}$. (Abstract truncated).Comment: 12 pages plus 9 figures, to be published in the Astrophysical Journal, v560, nr 1, pt 1 (Oct 10, 2001 issue

A STUDY ON DRUG UTILIZATION EVALUATION AND POTENTIAL DRUG RELATED PROBLEMS IN TYPE-2 DIABETES MELLITUS PATIENTS WITH CO-MORBIDITIES IN A TERTIARY CARE HOSPITAL

Objective: The objective of this study is to evaluate prescribing pattern, analyze drug-related problems, identify co-morbidities and complications in Type 2 Diabetes Mellitus patients and also to perform cost analysis of Biguanides, Sulfonylureas, Dipeptidyl Peptidase Inhibitors Methods: A Prospective observational study was done in General Medicine and Endocrinology Departments of PSG Hospitals. A total of 200 study subjects, including both inpatients and outpatients, above 18 y of age, prescribed with OHAs (Biguanides, Sulfonylureas and DPP4 inhibitors) were included in the study. Results: Diabetes was more prevalent among males. OHAs were most prescribed in the age group of 51-60 y. Hypertension (71%) was the most common comorbidity and Diabetic neuropathy (23%) was the most common complication found in the patients. Multidrug therapy (72.5%) was most prescribed in diabetic patients, followed by Biguanides. Hypoglycemia was the most prevalent ADR. Cost analysis showed that T. Linagliptin was of high cost and T. Glimepiride being the low cost. Using WHO core indicators prescribing patterns were assessed. Feedback was collected and results were reported to the physicians which showed rational utilization of drugs. Conclusion: The study on drug utilization conducted in a tertiary care hospital helped us to find out that prescribing trends seems to be progressing towards combination therapy, predominantly two-drug therap

Three-Dimensional Simulations of a Starburst-Driven Galactic Wind

We have performed a series of three-dimensional simulations of a starburst-driven wind in an inhomogeneous interstellar medium. The introduction of an inhomogeneous disk leads to differences in the formation of a wind, most noticeably the absence of the ``blow-out'' effect seen in homogeneous models. A wind forms from a series of small bubbles that propagate into the tenuous gas between dense clouds in the disk. These bubbles merge and follow the path of least resistance out of the disk, before flowing freely into the halo. Filaments are formed from disk gas that is broken up and accelerated into the outflow. These filaments are distributed throughout a biconical structure within a more spherically distributed hot wind. The distribution of the inhomogeneous interstellar medium in the disk is important in determining the morphology of this wind, as well as the distribution of the filaments. While higher resolution simulations are required in order to ascertain the importance of mixing processes, we find that soft X-ray emission arises from gas that has been mass-loaded from clouds in the disk, as well as from bow shocks upstream of clouds, driven into the flow by the ram pressure of the wind, and the interaction between these shocks.Comment: 37 pages, 16 figures, mpg movie can be obtained at http://www.mso.anu.edu.au/~jcooper/movie/video16.mpg, accepted for publication in Ap