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# Multiscale Part-Spectrum k-Distribution Database for Atomic Radiation in Hypersonic Nonequilibrium Flows

[+] Author and Article Information
Ankit Bansal

Department of Mechanical Engineering,  The Pennsylvania State University, University Park, PA 16802, e-mail: azb162@psu.edu

Michael Modest1

Fellow ASME School of Engineering,  University of California, Merced, Merced, CA 95343 e-mail: MModest@eng.ucmerced.edu

1

Corresponding author.

J. Heat Transfer 133(12), 122701 (Oct 07, 2011) (7 pages) doi:10.1115/1.4004528 History: Received July 24, 2010; Revised June 27, 2011; Published October 07, 2011; Online October 07, 2011

## Abstract

An accurate and compact part-spectrum k-distribution database has been developed for the two most important radiating species N and O encountered in hypersonic nonequilibrium flows. The database allows users to calculate the desired full-spectrum k-distributions through look-up and interpolation, providing an efficient means to perform radiative transfer calculations. A detailed methodology of the k-distribution data generation is presented. An optimized Gauss quadrature scheme is implemented for reducing the size of the database. The accuracy of the database is determined by comparing part-spectrum emissivities with those obtained from line-by-line calculations. The application of the database to construct full-spectrum k-distributions at arbitrary gas states is discussed. Heat transfer results for the stagnation line of the Stardust vehicle are discussed and CPU-time studies are presented, demonstrating the accuracy and efficiency of the k-distribution database.

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## Figures

Figure 1

Nonequilibrium Planck function (a) with overlap and (b) without overlap; ne  = 5.0 × 1015 cm−3 , Te  = 10,000 K, and T = 15,000 K

Figure 2

Sample part-spectrum k-distributions; ne  = 5.0 × 1015 cm−3 , Te  = 10,000 K, and T = 15,000 K

Figure 3

Part-spectrum emissivity; ϕ=.50, Te  = 10,000 K, and T = 15,000 K

Figure 4

Stardust stagnation line flow field (a) species number density and (b) temperature

Figure 5

Radiative heat source and absolute error along the Stardust stagnation line flow field

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