Foundation Performance of Very Old Structures

Withstanding the agents of destruction for several centuries, some of the structures in this world, exist as a testimony to the sound and perfected techniques of construction used in years that belong to the bygone past. Among the most famous are Taj Mahal and Qutb Minar, still standing in a magnificent and sound condition. One of the wonders of the world, Taj Mahal though built in seventeenth century still looks so fresh that the super-structure performance also speaks of the adequate and perfect foundation that must have been built for it. This paper deals with subsoil conditions at site, the type of foundation, its construction technique and its performance for a very long period for both Taj Mahal and Qutb Minar

Geotechnical Investigations for Foundation Design for Multi-storeyed Building

Oil and Natural Gas Commission of India plans to construct a multi-storeyed building in Dehradun city at the foothills of Himalayas. The geotechnical investigations were carried out at site to determine soil parameters for foundation design. It was found that it was not possible to provide a raft foundation for the building and hence alternatively the pile foundation was suggested. The pile load capacity was predicted on the basis of soil parameters determined and a comparison was then made with the results obtained by carrying out load tests on constructed piles

A Comparative Study of the Parker Instability under Three Models of the Galactic Gravity

To examine how non-uniform nature of the Galactic gravity might affect length and time scales of the Parker instability, we took three models of gravity, uniform, linear and realistic ones. To make comparisons of the three gravity models on a common basis, we first fixed the ratio of magnetic pressure to gas pressure at $\alpha$ = 0.25, that of cosmic-ray pressure at $\beta$ = 0.4, and the rms velocity of interstellar clouds at $a_s$ = 6.4 km s$^{-1}$, and then adjusted parameters of the gravity models in such a way that the resulting density scale heights for the three models may all have the same value of 160 pc. Performing linear stability analyses onto equilibrium states under the three models with the typical ISM conditions, we calculate the maximum growth rate and corresponding length scale for each of the gravity models. Under the uniform gravity the Parker instability has the growth time of 1.2$\times10^{8}$ years and the length scale of 1.6 kpc for symmetric mode. Under the realistic gravity it grows in 1.8$\times10^{7}$ years for both symmetric and antisymmetric modes, and develops density condensations at intervals of 400 pc for the symmetric mode and 200 pc for the antisymmetric one. A simple change of the gravity model has thus reduced the growth time by almost an order of magnitude and its length scale by factors of four to eight. These results suggest that an onset of the Parker instability in the ISM may not necessarily be confined to the regions of high $\alpha$ and $\beta$.Comment: Accepted for publication in ApJ, using aaspp4.sty, 18 text pages with 9 figure

The Leiodolide B Puzzle

Out of options? Even though a systematic approach was chosen, which led to a set of four diastereomeric macrolides modeled around the proposed structure of leiodolide B (see picture), the puzzle concerning the stereostructure of this cytotoxic metabolite derived from a deep-sea sponge still remains unsolved

Taj Mahal – An Appraisal of Foundation Performance

Because of severe restrictions placed by the National Authority, no authentic data on subsoil details below Taj Mahal - a protected monument - is available. For the first time, an attempt has been made to fill in gaps that exist in our knowledge of subsoil profile below the structure and present a plausible appraisal of foundation performance during the existence of the structure. Since details of foundations cited in literature on Taj Mahal really fall into the realms of architectural conjecture, in the present analysis, engineering intuition and judgement have gone into making certain premises regarding the probable type, dimensions and the depth of the existing foundations of Taj Mahal. These premises, complimented by borehole data and laboratory tests have enabled the assessment of the foundation performance to be made in as realistic a manner as is practically possible

NMA CO (J=1-0) Observations of the Halpha/Radio Lobe Galaxy NGC 3079: Gas Dynamics in a Weak Bar Potential and Central Massive Core

within 24 lines with 80 characters) We present ^12CO (1-0) observations in the central 4.5 kpc (1 arcmin) of the Halpha/Radio lobe galaxy NGC 3079 with the Nobeyama Millimeter Array. The molecular gas shows four components: a main disk, spiral arms, a nuclear disk, and a nuclear core. The main disk extends beyond our spatial coverage. The spiral arms are superimposed on the main disk. The nuclear disk with about 600 pc radius has an intense concentration of molecular gas. Its appearance on PV diagrams is indicative of oval motions of the gas, rather than circular. The nuclear core is more compact than our resolution. Though it is unresolved, the nuclear core shows a very high velocity about 200 km/s even at the radius of about 100 pc on the PV diagram. We propose a model that NGC 3079 contains a weak bar. This model explains the observed features: the main disk and spiral arms result from gaseous x1-orbits and associated crowding respectively. The nuclear disk arises from gaseous x2-orbits. From the appearance of the spiral arms on the PV diagram, the pattern speed of the bar is estimated to be 55+-10 km/s/kpc. The high velocity of the nuclear core cannot be explained by our model for a bar. Thus we attribute it to a central massive core with a dynamical mass of 10^9 Msun within the central 100 pc. This mass is three orders of magnitude more massive than that of a central black hole in this galaxy.Comment: 43 pages, 17 figures; ApJ, 573, 105, 200

Radio and gamma-ray constraints on dark matter annihilation in the Galactic center

We determine upper limits on the dark matter (DM) self-annihilation cross section for scenarios in which annihilation leads to the production of electron--positron pairs. In the Galactic centre (GC), relativistic electrons and positrons produce a radio flux via synchroton emission, and a gamma ray flux via bremsstrahlung and inverse Compton scattering. On the basis of archival, interferometric and single-dish radio data, we have determined the radio spectrum of an elliptical region around the Galactic centre of extent 3 degrees semi-major axis (along the Galactic plane) and 1 degree semi-minor axis and a second, rectangular region, also centered on the GC, of extent 1.6 degrees x 0.6 degrees. The radio spectra of both regions are non-thermal over the range of frequencies for which we have data: 74 MHz -- 10 GHz. We also consider gamma-ray data covering the same region from the EGRET instrument (about GeV) and from HESS (around TeV). We show how the combination of these data can be used to place robust constraints on DM annihilation scenarios, in a way which is relatively insensitive to assumptions about the magnetic field amplitude in this region. Our results are approximately an order of magnitude more constraining than existing Galactic centre radio and gamma ray limits. For a DM mass of m_\chi =10 GeV, and an NFW profile, we find that the velocity-averaged cross-section must be less than a few times 10^-25 cm^3 s^-1.Comment: 14 pages, 9 figures. Version accepted for publication in PRD. Reference section updated/extended