The Effect of Thermal Parameters on the Flow Temperature of a Magnetized Plasma in a Sphere
International Journal of Astrophysics and Space Science
Volume 7, Issue 3, June 2019, Pages: 39-44
Received: Jul. 19, 2019; Accepted: Aug. 29, 2019; Published: Sep. 18, 2019
Views 89      Downloads 6
Authors
Tuduo Biepremene Sebastian, Department of Physics, University of Port Harcourt, Port Harcourt, Nigeria
Abbey Tamunoimi Michael, Department of Physics, University of Port Harcourt, Port Harcourt, Nigeria
Alagoa Kingsley D., Department of Physics, Niger Delta University, Amassoma, Nigeria
Onwuneme Sylvester Ebere, Department of Physics, University of Port Harcourt, Port Harcourt, Nigeria
Article Tools
Follow on us
Abstract
The effect of thermal parameters on the flow temperature of a magnetized plasma in a sphere was studied. The study models astrophysical environments such as the Sun, which have spherical outline. The governing equations of the problem were obtained based on the Navier-Stokes equations under the Boussinesq’s approximation. The solutions to the resulting equations were sought by means of the general perturbation method and the results were graphically represented with radial distance, r = 1.0 on the figures corresponding to the surface of the sphere. The thermal parameters; particularly, the radiation parameter, N2 and free convection parameter, Gr. were investigated in this study with a view to determine the effect of varying these parameters on the plasma flow temperature. Increasing both N2 and Gr. led to a decrease in the plasma flow temperature in the sphere. However, above the sphere (i.e. at radial distances, r >1.0) where the plasma density is sparse, increasing N2 and Gr. produced a corresponding increase in the plasma flow temperature. The decrease in the plasma flow temperature within the sphere with increase in the thermal parameters was observed to be more significant between radial distances, r = 0.25 and r = 0.7 (i.e., 0.25 ≤ r ≤ 0.7) than between r = 0.7 and r = 1.0 (i.e., 0.7 ≤ r ≤ 1.0). This is attributable to the prevalence of partially ionized heavy elements within 0.7 ≤ r ≤ 1.0 (corresponding to the convection zone of the solar interior) which trap the high energy photons thereby reducing the rate of radiative heat loss.
Keywords
Thermal Parameters, Flow Temperature, Magnetized Plasma
To cite this article
Tuduo Biepremene Sebastian, Abbey Tamunoimi Michael, Alagoa Kingsley D., Onwuneme Sylvester Ebere, The Effect of Thermal Parameters on the Flow Temperature of a Magnetized Plasma in a Sphere, International Journal of Astrophysics and Space Science. Vol. 7, No. 3, 2019, pp. 39-44. doi: 10.11648/j.ijass.20190703.12
Copyright
Copyright © 2019 Authors retain the copyright of this article.
This article is an open access article distributed under the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0/) which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
References
[1]
Alagoa, K. D., Tay, G. and Abbey, T. M. (1999). Radiative and free convective effects of a MHD flow through a porous medium between infinite parallel plates with time-dependent suction. Astrophysics and Space Science, 260: 455-468.
[2]
Abbey, T. M. (2004). Effect of radiative heat transfer, free convection and time dependent suction on the flow of a two-component plasma in a porous medium sandwich between two infinite parallel plates. (Workshop proceedings) International Centre for Theoretical Physics, Trieste, Italy.
[3]
Abbey, T. M. (2005). The flow of a two-component plasma past a rotating hot sphere with an oscillating diameter, workshop proceedings. (Workshop proceedings) International Centre for Theoretical Physics, Trieste, Italy.
[4]
Roger, B. P. and Robert, C. J. (2016). Solar Physics and Terrestrial Effects: A Curriculum Guide for Teachers, Grade 7-12. (Third Edition), Space Weather Prediction Center, National Oceanic and Atmospheric Administration.
[5]
Abbey, T. M., Bestman, A. R. and Mbeledogu, I. U. (1992). The flow of atwo-component plasma model in a porous rotating hot sphere. Astrophysics and Space Science, 197: 61-76.
[6]
Abbey, T. M. and Bestman, A. R. (1995). Slip flow in a two-component plasma model with radiative heat transfer. International Journal of Energy Research, 19: 1-6.
[7]
Abbey, T. M. (1996). The flow of a two-component plasma model past a rotating porous hot sphere. Nigerian Journal of Physics, 8S: 51-60.
[8]
Sasikumar, J. and Govindarjan, A. (2016). Effect of heat and mass transfer on MHD oscillatory flow with chemical reaction and slip conditions in asymmetric wavy channel. Journal of Engineering and Applied Sciences, 11 (2): 1164-1170.
[9]
Sanatan, D., Mrinal, J. and Rabindra, N. J. (2011). Radiation effect on natural convection near a vertical plate embedded in porous medium with ramped wall temperature, Open J. of Fluid Dynamics, 1: 1–11.
[10]
Priest, E. R. (1982). Solar magneto-hydrodynamics 1. Dordrecht, Holland: D. Reidel Publishing Company.
[11]
Sherman, F. S. (1990). Viscous flow. (International Edition) New York City, NY: McGeaw-Hill. ISBN: 0-07-056579-1.
[12]
Alagoa, K. D. and Sakanaka, P. H. (1998). Gravitational stability of the solar plasma. International Centre for Theoretical Physics, Trieste, Italy. IC/98/112.
[13]
Alagoa, K. D. and Abbey, T. M. (2001). Temperature distribution in the solar globe due to exponentially varying plasma density. Mathematical Science Forum, 3: 1-8.
[14]
Abbey, T. M. and John, E. (2000). Transient Slip flow in a two-component plasma model with radiative heat transfer. Mathematical Science Forum, 2: 37-47.
[15]
Bestman, A. R. (1983). Low Reynolds number flow in a heated tube of varying section. Journal of the Australian Mathematical Society Series, B25: 244-260.
[16]
He, J.-H. (2006). Some asymptotic methods for strongly nonlinear equations. International Journal of Modern Physics B, 20 (10): 1141-1199.
[17]
Biazar, J. and Eslami, M. (2011). A new homotopy perturbation method for solving systems of partial differential equations. Computers and Mathematics with Applications, 62: 225-234.
[18]
Molliq, Y. R. and Noorani, M. S. M. (2012). Solving the Fractional Rosenau-Hyman Equation via Variational Iteration Method and Homotopy Perturbation Method. International Journal of Differential Equations, 2012 (ID 472030): 1-14.
[19]
Biazar, J. and Eslami, M. (2010). Analytic solutions for telegraph equation by differential transform method. Physics Letters A, 374: 2904-2906.
[20]
Bailey, J. E., Rochau, G. A., Mancini, R. C., Iglesias, C. A., MacFarlane, J. J., Golovkin, I., Blancard, C., Colgan, J., Ph. Cosse and Faussurier, G. (2009). Experimental investigation of opacity models for stellar interior, inertial fusion and high energy density plasmas. Physics of plasmas, 16: 058101.
[21]
Hanasoge, S., Gizon, L. and Katepalli, R. S. (2015). Seismic Sounding of Convection in the Sun. Retrieved from: https://arxiv.org/pdf/1503.07961.pdf.
[22]
Krief, M., Feigel, A. and Gazit, D. (2016). Line Broadening and the Solar Opacity Problem. Astrophysical Journal, 824: 98 (pp6).
ADDRESS
Science Publishing Group
1 Rockefeller Plaza,
10th and 11th Floors,
New York, NY 10020
U.S.A.
Tel: (001)347-983-5186