A bounded upwinding scheme for computing convection-dominated transport problems

A practical high resolution upwind differencing scheme for the numerical solution of convection-dominated transport problems is presented. The scheme is based on TVD and CBC stability criteria and is implemented in the context of the finite difference methodology. The performance of the scheme is investigated by solving the 1D/2D scalar advection equations, 1D inviscid Burgers’ equation, 1D scalar convection–diffusion equation, 1D/2D compressible Euler’s equations, and 2D incompressible Navier–Stokes equations. The numerical results displayed good agreement with other existing numerical and experimental data

Manajemen Ekosistem Pesisir Pulau-Pulau Kecil Untuk Ekowisata Berkelanjutan Di Pulau Saparua

Saparua as small island rich in coastal natural resources. Main coastal ecosystem are mangrove, seagrass beds, coral reefs and sandy beach. Coastal ecosystem also has an important role in ecotourism environment services to improve the communities economy and must be managed sustainably. This paper aimed to identifying potential small islands coastal areas as a tourist destination and planned management to sustainable ecotourism used SWOT analysis. Ecotourism was sustained in small islands can be conducted integrally through 14 management strategy to tourism industry which economic, social and environmental dimension. Ecotourism coastal area management of small islands should be done in coordination with the agrosilvofishery

Caracterização de nove genótipos de milho (Zea mays L.) en relação à área foliar e coeficiente de extinção de luz

A field experiment was carried out to evaluate nine corn genotypes (Arichuna, Baraure, B raquitico, Expe-rimental-2, Foremaiz PB, FM-6, Obregón, Proseca-71 and Tocorón) in relation to: mean leaf area per plant, total leaf area per plant (TLA), leaf area index (LAI), grain yield (Y) and light extinction coefficient (K) at 0.50m, 1.00m, 1.50m, 2.00m and 2.50m of plant height (from soil to flag leaf). Also, correlation and single regression between LAI and yield was performed. Significant genotypical differences for all variables were found, except for mean leaf area per plant Ranging was: mean leaf area per plant (471 cm² for Foremaiz PB and 606 cm² for Baraure); TLA (5,327 cm² for Foremaiz PB and 8,411 for Braquítico); LAI (4.26, Foremaiz PB and 6.67, Braquítico); K (0.23 for Braquítico and 0.42, Arichuna); Y (2, 877, Braquítico and 4,784 kg.ha-1 for Tocoron).The relationship between Y and LAI was not significant (r = 0.07). The relationship of LAI and K was described very well by Beer's law.Se caracterizaron nueve materiales genéticos de maíz (Arichuna, Baraure, Braquítico, Experimental-2, Foremaíz PB, FM-6, Obregón, Proscca-71 y Tocorón), en relación con área promedio de hoja por planta, área foliar total por planta (AFT), índice de área foliar (IAF), y coeficiente de extinción de luz (K) a 0,50 m, 1,00 m, 1,50 m, 2,00 m y 2,50 m de altura de la planta (medidos a partir del suelo). Además, estudios de correlación y regresión simple fueron hechos entre rendimiento (R) y IAF. Se encontraron rangos de variación para las diversas variables: Area promedio de hoja por planta(471cm² para Foremaiz PB y 606 cm² para Baraure); AFT ( 5 327cm² en Foremaiz PB y 8 411 cm² para Braquítico); IAF (4,26, Foremaiz PB y 6,67, Braquítico); K (0,23 para Braquítico y 0,42, Arichuna); rendimiento (2 877 kg.ha-1, Braquítico y 4 784 kg.ha-1 en Tocorón). La relación entre rendimiento y IAF no fue significativa(r = 0,07). La asociación de IAF y K file muy bien descrita por la ley de Beer.Foram caracterizados nove materiais genéticos de milho (Arichuna, Baraure, Braquítico, Experimental-2, Foremaíz PB, FM-6, Obregón, Proseca-71 y Tocorón) com relação a área foliar média de folhas por planta(AF), área foliar total por planta (AFT), índice de área foliar (IAF) e coeficiente de extinção de luz (K) a 0,50m, 1,00m, 1,50m, 2,00m e 2,50m de altura (a partir do solo). Foram encontrados os seguintes intervalos de variação para as diversas variáveis: área média de folhas por planta (471 cm² para Foremaíz PB e 606 cm² Baraure); área foliar total por planta: 5 327 cm² (Foremaiz PB) e 8 411 cm² (Braquítico), índice de área foliar: 4,26 (Foremaiz PB) e 6,67 (Braquítico); coeficiente de extinção de luz: 0,23 (Braquítico) e 0,42 (Arichuna); rendimento: 2 877 kg.ha-1 (Braquítico) e 4 784 kg.ha-1 (Tocorón). Não foi encontrada relação entre o rendimento e o IAF (r = 0,07), e a associação do IAF e K foi muito bem explicada pela lei de Beer

Thermal stability of sputter-deposited 330 austenitic stainless-steel thin films with nanoscale growth twins

We have explored the thermal stability of nanoscale growth twins in sputter-deposited 330 stainless-steel (SS) films by vacuum annealing up to 500 °C. In spite of an average twin spacing of only 4 nm in the as-deposited films, no detectable variation in the twin spacing or orientation of twin interfaces was observed after annealing. An increase in the average columnar grain size was observed after annealing. The hardness of 330 SS films increases after annealing, from 7 GPa for as-deposited films to around 8 GPa for annealed films, while the electrical resistivity decreases slightly after annealing. The changes in mechanical and electrical properties after annealing are interpreted in terms of the corresponding changes in the residual stress and microstructure of the films

Accelerating Universe from an Evolving Lambda in Higher Dimension

We find exact solutions in five dimensional inhomogeneous matter dominated model with a varying cosmological constant. Adjusting arbitrary constants of integration one can also achieve acceleration in our model. Aside from an initial singularity our spacetime is regular everywhere including the centre of the inhomogeneous distribution. We also study the analogous homogeneous universe in (4+d) dimensions. Here an initially decelerating model is found to give late acceleration in conformity with the current observational demands. We also find that both anisotropy and number of dimensions have a role to play in determining the time of flip, in fact the flip is delayed in multidimensional models. Some astrophysical parameters like the age, luminosity distance etc are also calculated and the influence of extra dimensions is briefly discussed. Interestingly our model yields a larger age of the universe compared to many other quintessential models.Comment: 18 pages, 9 figure

Einstein energy associated with the Friedmann -Robertson -Walker metric

Following Einstein's definition of Lagrangian density and gravitational field energy density (Einstein, A., Ann. Phys. Lpz., 49, 806 (1916); Einstein, A., Phys. Z., 19, 115 (1918); Pauli, W., {\it Theory of Relativity}, B.I. Publications, Mumbai, 1963, Trans. by G. Field), Tolman derived a general formula for the total matter plus gravitational field energy ($P_0$) of an arbitrary system (Tolman, R.C., Phys. Rev., 35(8), 875 (1930); Tolman, R.C., {\it Relativity, Thermodynamics & Cosmology}, Clarendon Press, Oxford, 1962)); Xulu, S.S., arXiv:hep-th/0308070 (2003)). For a static isolated system, in quasi-Cartesian coordinates, this formula leads to the well known result $P_0 = \int \sqrt{-g} (T_0^0 - T_1^1 -T_2^2 -T_3^3) ~d^3 x$, where $g$ is the determinant of the metric tensor and $T^a_b$ is the energy momentum tensor of the {\em matter}. Though in the literature, this is known as "Tolman Mass", it must be realized that this is essentially "Einstein Mass" because the underlying pseudo-tensor here is due to Einstein. In fact, Landau -Lifshitz obtained the same expression for the "inertial mass" of a static isolated system without using any pseudo-tensor at all and which points to physical significance and correctness of Einstein Mass (Landau, L.D., and Lifshitz, E.M., {\it The Classical Theory of Fields}, Pergamon Press, Oxford, 2th ed., 1962)! For the first time we apply this general formula to find an expression for $P_0$ for the Friedmann- Robertson -Walker (FRW) metric by using the same quasi-Cartesian basis. As we analyze this new result, physically, a spatially flat model having no cosmological constant is suggested. Eventually, it is seen that conservation of $P_0$ is honoured only in the a static limit.Comment: By mistake a marginally different earlier version was loaded, now the journal version is uploade

High-redshift objects and the generalized Chaplygin gas

Motivated by recent developments in particle physics and cosmology, there has been growing interest in an unified description of dark matter and dark energy scenarios. In this paper we explore observational constraints from age estimates of high-$z$ objects on cosmological models dominated by an exotic fluid with equation of state $p = -A/\rho^{\alpha}$ (the so-called generalized Chaplygin gas) which has the interesting feature of interpolating between non-relativistic matter and negative-pressure dark energy regimes. As a general result we find that, if the age estimates of these objects are correct, they impose very restrictive limits on some of these scenarios.Comment: 5 pages, 3 figures, to appear in Phys. Rev.

Constraining the dark energy with galaxy clusters X-ray data

The equation of state characterizing the dark energy component is constrained by combining Chandra observations of the X-ray luminosity of galaxy clusters with independent measurements of the baryonic matter density and the latest measurements of the Hubble parameter as given by the HST key project. By assuming a spatially flat scenario driven by a "quintessence" component with an equation of state $p_x = \omega \rho_x$ we place the following limits on the cosmological parameters $\omega$ and $\Omega_{\rm{m}}$: (i) $-1 \leq \omega \leq -0.55$ and $\Omega_{\rm m} = 0.32^{+0.027}_{-0.014}$ (1$\sigma$) if the equation of state of the dark energy is restricted to the interval $-1 \leq \omega < 0$ (\emph{usual} quintessence) and (ii) $\omega = -1.29^{+0.686}_{-0.792}$ and $\Omega_{\rm{m}} = 0.31^{+0.037}_{-0.034}$ ($1\sigma$) if $\omega$ violates the null energy condition and assume values $< -1$ (\emph{extended} quintessence or ``phantom'' energy). These results are in good agreement with independent studies based on supernovae observations, large-scale structure and the anisotropies of the cosmic background radiation.Comment: 6 pages, 4 figures, LaTe

Bianchi Type-I Cosmological Models with Variable G and 4\Lambda$-Terms in General Relativity

Einstein's field equations with variable gravitational and cosmological ``constant'' are considered in presence of perfect fluid for Bianchi type-I spacetime. Consequences of the four cases of the phenomenological decay of $\Lambda$ have been discussed which are consistent with observations. The physical significance of the cosmological models have also been discussed.Comment: 12 pages, no figur