The Effect of Thermal Parameters on the Flow Temperature of a Magnetized Plasma in a Sphere

Tuduo Biepremene Sebastian; Abbey Tamunoimi Michael; Alagoa Kingsley D.; Onwuneme Sylvester Ebere

doi:doi:10.11648/j.ijass.20190703.12

| Peer-Reviewed

The Effect of Thermal Parameters on the Flow Temperature of a Magnetized Plasma in a Sphere

Tuduo Biepremene Sebastian, Abbey Tamunoimi Michael, Alagoa Kingsley D., Onwuneme Sylvester Ebere

Published in International Journal of Astrophysics and Space Science (Volume 7, Issue 3)

Received: 19 July 2019 Accepted: 29 August 2019 Published: 18 September 2019

Views: Downloads:

Download PDF

Share This Article

Twitter
Linked In
Facebook

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.

Published in	International Journal of Astrophysics and Space Science (Volume 7, Issue 3)
DOI	10.11648/j.ijass.20190703.12
Page(s)	30-35
Creative Commons	This is an Open Access article, distributed under the terms of the Creative Commons Attribution 4.0 International License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted use, distribution and reproduction in any medium or format, provided the original work is properly cited.
Copyright	Copyright © The Author(s), 2019. Published by Science Publishing Group

Keywords

Thermal Parameters, Flow Temperature, Magnetized Plasma

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).

Cite This Article

Plain Text BibTeX RIS

APA Style

Tuduo Biepremene Sebastian, Abbey Tamunoimi Michael, Alagoa Kingsley D., Onwuneme Sylvester Ebere. (2019). The Effect of Thermal Parameters on the Flow Temperature of a Magnetized Plasma in a Sphere. International Journal of Astrophysics and Space Science, 7(3), 30-35. https://doi.org/10.11648/j.ijass.20190703.12

Copy | Download

ACS Style

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. Int. J. Astrophys. Space Sci. 2019, 7(3), 30-35. doi: 10.11648/j.ijass.20190703.12

Copy | Download

AMA Style

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. Int J Astrophys Space Sci. 2019;7(3):30-35. doi: 10.11648/j.ijass.20190703.12

Copy | Download

@article{10.11648/j.ijass.20190703.12,
  author = {Tuduo Biepremene Sebastian and Abbey Tamunoimi Michael and Alagoa Kingsley D. and Onwuneme Sylvester Ebere},
  title = {The Effect of Thermal Parameters on the Flow Temperature of a Magnetized Plasma in a Sphere},
  journal = {International Journal of Astrophysics and Space Science},
  volume = {7},
  number = {3},
  pages = {30-35},
  doi = {10.11648/j.ijass.20190703.12},
  url = {https://doi.org/10.11648/j.ijass.20190703.12},
  eprint = {https://article.sciencepublishinggroup.com/pdf/10.11648.j.ijass.20190703.12},
  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.},
 year = {2019}
}

Copy | Download

TY - JOUR
T1 - The Effect of Thermal Parameters on the Flow Temperature of a Magnetized Plasma in a Sphere
AU - Tuduo Biepremene Sebastian
AU - Abbey Tamunoimi Michael
AU - Alagoa Kingsley D.
AU - Onwuneme Sylvester Ebere
Y1 - 2019/09/18
PY - 2019
N1 - https://doi.org/10.11648/j.ijass.20190703.12
DO - 10.11648/j.ijass.20190703.12
T2 - International Journal of Astrophysics and Space Science
JF - International Journal of Astrophysics and Space Science
JO - International Journal of Astrophysics and Space Science
SP - 30
EP - 35
PB - Science Publishing Group
SN - 2376-7022
UR - https://doi.org/10.11648/j.ijass.20190703.12
AB - 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.
VL - 7
IS - 3
ER -

Copy | Download

Author Information

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

Download PDF

Sections

Plain Text BibTeX RIS

APA Style

Tuduo Biepremene Sebastian, Abbey Tamunoimi Michael, Alagoa Kingsley D., Onwuneme Sylvester Ebere. (2019). The Effect of Thermal Parameters on the Flow Temperature of a Magnetized Plasma in a Sphere. International Journal of Astrophysics and Space Science, 7(3), 30-35. https://doi.org/10.11648/j.ijass.20190703.12

Copy | Download

ACS Style

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. Int. J. Astrophys. Space Sci. 2019, 7(3), 30-35. doi: 10.11648/j.ijass.20190703.12

Copy | Download

AMA Style

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. Int J Astrophys Space Sci. 2019;7(3):30-35. doi: 10.11648/j.ijass.20190703.12

Copy | Download

@article{10.11648/j.ijass.20190703.12,
  author = {Tuduo Biepremene Sebastian and Abbey Tamunoimi Michael and Alagoa Kingsley D. and Onwuneme Sylvester Ebere},
  title = {The Effect of Thermal Parameters on the Flow Temperature of a Magnetized Plasma in a Sphere},
  journal = {International Journal of Astrophysics and Space Science},
  volume = {7},
  number = {3},
  pages = {30-35},
  doi = {10.11648/j.ijass.20190703.12},
  url = {https://doi.org/10.11648/j.ijass.20190703.12},
  eprint = {https://article.sciencepublishinggroup.com/pdf/10.11648.j.ijass.20190703.12},
  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.},
 year = {2019}
}

Copy | Download