MHD Fluid Flow of an Exponentially Varying Plasma Density in a Radiating and Slowly Rotating Hot Sphere

B. S. Tuduo; T. M. Abbey; K. D. Alagoa

doi:doi:10.11648/j.ijass.20180601.12

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MHD Fluid Flow of an Exponentially Varying Plasma Density in a Radiating and Slowly Rotating Hot Sphere

B. S. Tuduo, T. M. Abbey, K. D. Alagoa

Published in International Journal of Astrophysics and Space Science (Volume 6, Issue 1)

Received: 15 June 2017 Accepted: 6 July 2017 Published: 11 February 2018

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Abstract

The study presents the effect of density variation on the flow structure of a plasma gas in a slowly rotating and radiating hot sphere. The problem which is solved by general perturbation method shows that the plasma temperature decreases to a minimum at a radial distance of 1.4 solar radii and then increased to a maximum value at a radial distance of 3.5 solar radii, for various radiation parameters, N2. The sudden increase in temperature profile when the radial distance is 1.4 solar radii, indicates the heating up of the upper regions of the solar atmosphere.

Published in	International Journal of Astrophysics and Space Science (Volume 6, Issue 1)
DOI	10.11648/j.ijass.20180601.12
Page(s)	18-27
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), 2018. Published by Science Publishing Group

Keywords

MHD Flow, Exponentially Varying Plasma Density, Radiating Hot Sphere

References

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[6]	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.
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APA Style

B. S. Tuduo, T. M. Abbey, K. D. Alagoa. (2018). MHD Fluid Flow of an Exponentially Varying Plasma Density in a Radiating and Slowly Rotating Hot Sphere. International Journal of Astrophysics and Space Science, 6(1), 18-27. https://doi.org/10.11648/j.ijass.20180601.12

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ACS Style

B. S. Tuduo; T. M. Abbey; K. D. Alagoa. MHD Fluid Flow of an Exponentially Varying Plasma Density in a Radiating and Slowly Rotating Hot Sphere. Int. J. Astrophys. Space Sci. 2018, 6(1), 18-27. doi: 10.11648/j.ijass.20180601.12

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AMA Style

B. S. Tuduo, T. M. Abbey, K. D. Alagoa. MHD Fluid Flow of an Exponentially Varying Plasma Density in a Radiating and Slowly Rotating Hot Sphere. Int J Astrophys Space Sci. 2018;6(1):18-27. doi: 10.11648/j.ijass.20180601.12

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@article{10.11648/j.ijass.20180601.12,
  author = {B. S. Tuduo and T. M. Abbey and K. D. Alagoa},
  title = {MHD Fluid Flow of an Exponentially Varying Plasma Density in a Radiating and Slowly Rotating Hot Sphere},
  journal = {International Journal of Astrophysics and Space Science},
  volume = {6},
  number = {1},
  pages = {18-27},
  doi = {10.11648/j.ijass.20180601.12},
  url = {https://doi.org/10.11648/j.ijass.20180601.12},
  eprint = {https://article.sciencepublishinggroup.com/pdf/10.11648.j.ijass.20180601.12},
  abstract = {The study presents the effect of density variation on the flow structure of a plasma gas in a slowly rotating and radiating hot sphere. The problem which is solved by general perturbation method shows that the plasma temperature decreases to a minimum at a radial distance of 1.4 solar radii and then increased to a maximum value at a radial distance of 3.5 solar radii, for various radiation parameters, N2. The sudden increase in temperature profile when the radial distance is 1.4 solar radii, indicates the heating up of the upper regions of the solar atmosphere.},
 year = {2018}
}

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TY  - JOUR
T1  - MHD Fluid Flow of an Exponentially Varying Plasma Density in a Radiating and Slowly Rotating Hot Sphere
AU  - B. S. Tuduo
AU  - T. M. Abbey
AU  - K. D. Alagoa
Y1  - 2018/02/11
PY  - 2018
N1  - https://doi.org/10.11648/j.ijass.20180601.12
DO  - 10.11648/j.ijass.20180601.12
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  - 18
EP  - 27
PB  - Science Publishing Group
SN  - 2376-7022
UR  - https://doi.org/10.11648/j.ijass.20180601.12
AB  - The study presents the effect of density variation on the flow structure of a plasma gas in a slowly rotating and radiating hot sphere. The problem which is solved by general perturbation method shows that the plasma temperature decreases to a minimum at a radial distance of 1.4 solar radii and then increased to a maximum value at a radial distance of 3.5 solar radii, for various radiation parameters, N2. The sudden increase in temperature profile when the radial distance is 1.4 solar radii, indicates the heating up of the upper regions of the solar atmosphere.
VL  - 6
IS  - 1
ER  -

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Author Information

B. S. Tuduo

Department of Physics, University of Port Harcourt, Port Harcourt, Nigeria
T. M. Abbey

Department of Physics, University of Port Harcourt, Port Harcourt, Nigeria
K. D. Alagoa

Department of Physics, Niger Delta University, Amassoma, Nigeria

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APA Style

B. S. Tuduo, T. M. Abbey, K. D. Alagoa. (2018). MHD Fluid Flow of an Exponentially Varying Plasma Density in a Radiating and Slowly Rotating Hot Sphere. International Journal of Astrophysics and Space Science, 6(1), 18-27. https://doi.org/10.11648/j.ijass.20180601.12

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ACS Style

B. S. Tuduo; T. M. Abbey; K. D. Alagoa. MHD Fluid Flow of an Exponentially Varying Plasma Density in a Radiating and Slowly Rotating Hot Sphere. Int. J. Astrophys. Space Sci. 2018, 6(1), 18-27. doi: 10.11648/j.ijass.20180601.12

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AMA Style

B. S. Tuduo, T. M. Abbey, K. D. Alagoa. MHD Fluid Flow of an Exponentially Varying Plasma Density in a Radiating and Slowly Rotating Hot Sphere. Int J Astrophys Space Sci. 2018;6(1):18-27. doi: 10.11648/j.ijass.20180601.12

Copy | Download

@article{10.11648/j.ijass.20180601.12,
  author = {B. S. Tuduo and T. M. Abbey and K. D. Alagoa},
  title = {MHD Fluid Flow of an Exponentially Varying Plasma Density in a Radiating and Slowly Rotating Hot Sphere},
  journal = {International Journal of Astrophysics and Space Science},
  volume = {6},
  number = {1},
  pages = {18-27},
  doi = {10.11648/j.ijass.20180601.12},
  url = {https://doi.org/10.11648/j.ijass.20180601.12},
  eprint = {https://article.sciencepublishinggroup.com/pdf/10.11648.j.ijass.20180601.12},
  abstract = {The study presents the effect of density variation on the flow structure of a plasma gas in a slowly rotating and radiating hot sphere. The problem which is solved by general perturbation method shows that the plasma temperature decreases to a minimum at a radial distance of 1.4 solar radii and then increased to a maximum value at a radial distance of 3.5 solar radii, for various radiation parameters, N2. The sudden increase in temperature profile when the radial distance is 1.4 solar radii, indicates the heating up of the upper regions of the solar atmosphere.},
 year = {2018}
}

Copy | Download

TY  - JOUR
T1  - MHD Fluid Flow of an Exponentially Varying Plasma Density in a Radiating and Slowly Rotating Hot Sphere
AU  - B. S. Tuduo
AU  - T. M. Abbey
AU  - K. D. Alagoa
Y1  - 2018/02/11
PY  - 2018
N1  - https://doi.org/10.11648/j.ijass.20180601.12
DO  - 10.11648/j.ijass.20180601.12
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  - 18
EP  - 27
PB  - Science Publishing Group
SN  - 2376-7022
UR  - https://doi.org/10.11648/j.ijass.20180601.12
AB  - The study presents the effect of density variation on the flow structure of a plasma gas in a slowly rotating and radiating hot sphere. The problem which is solved by general perturbation method shows that the plasma temperature decreases to a minimum at a radial distance of 1.4 solar radii and then increased to a maximum value at a radial distance of 3.5 solar radii, for various radiation parameters, N2. The sudden increase in temperature profile when the radial distance is 1.4 solar radii, indicates the heating up of the upper regions of the solar atmosphere.
VL  - 6
IS  - 1
ER  -

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