Handbook of Numerical Heat Transfer Free Full Download Links from Multiple Mirrors added by DL4W on 2015-04-10 02:13:35. Handbook of heat transfer / editors, W.M. Rohsenow, J.P. Hartnett. Y.I. Cho. m 3rd ed. p. cm. Includes bibliographical references and index. ISBN 0-07053555-8. Students investigate heat transfer by conduction, convection and radiation. The analogy between heat and mass transfer is covered and applied in the analysis.

Handbook of heat transfer

Coal pyrolysis: Experiments, kinetic rates and mechanisms

Components, formulations, solutions, evaluation, and application of comprehensive combustion models

A parametric study of radiative heat transfer in pulverised coal furnaces

We present a detailed study of the circumstellar envelope of the post-asymptotic giant branch "21 µm object" HD 56126. We build a detailed dust radiative transfer model of the circumstellar envelope in order to derive the dust composi- tion and mass, and the mass-loss history of the star. To model the emission of the dust we use amorphous carbon, hydrogenated amorphous carbon, magnesium sulfide and titanium carbide. We present a detailed parametrisation of the optical properties of hydrogenated amorphous carbon as a function of H/C content. The mid-infrared imaging and spectroscopy is best reproduced by a single dust shell from 1.2 to 2.6 �� radius around the central star. This shell originates from a short period during which the mass-loss rate exceeded 10 −4 M� /yr. We find that the strength of the "21" µm feature poses a problem for the TiC identification. The low abundance of Ti requires very high absorption cross-sections in the ultraviolet and visible wavelength range to explain the strength of the feature. Other nano-crystalline metal carbides should be considered as well. We find that hydrogenated amor- phous carbon in radiative equilibrium with the local radiation field does not reach a high enough temperature to explain the strength of the 3.3-3.4 and 6-9 µm hydrocarbon features relative to the 11-17 µm hydrocarbon features. We propose that the carriers of these hydrocarbon features are not in radiative equilibrium but are transiently heated to high temperature. We find that 2 per cent of the dust mass is required to explain the strength of the "30" µm feature, which fits well within the measured atmospheric abundance of Mg and S. This further strengthens the MgS identification of the "30" µm feature.

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The circumstellar envelope of the C-rich post-AGB star HD 56126

The infrared optical constants, n and k, (n = n-ik) of swelling and nonswelling coals, their respective char products, and limestone at room temperature have been obtained by a particle extinction technique using compressed KBr tables. By assuming spherical particles and using Mie theory for the particle extinction measurements in conjunction with normal specular reflectance measurements from polished specimens, it is possible to obtain more accurate values for n and k than if the usual Fresnel reflectance technique is misapplied to samples that may appear specular but do not satisfy the stringent conditions necessary for invoking the Fresnel equations. Values of k for coal were found to be an order-of-magnitude smaller than previously reported values, with absorption due mainly to molecular vibration. The results for char evidenced that a significant increase in absorption by free electrons takes place upon devolatization and carbonization of coal. The limestone results demonstrated pronounced molecular absorption bands characteristic of CaCO/sub 3/.

T. Kunitomo

Papers

The Optical Constants of Coal, Char, and Limestone