Astrophysics and Space Science

, Volume 92, Issue 2, pp 359–364 | Cite as

The emergence of a spherical magnetogasdynamic shock wave at the surface of a star

  • R. C. Srivastava
Article

Abstract

The propagation of a magnetogasdynamic shock wave originating in a stellar interior, is ocnsidered when it approaches the surfaces of the star. The flow behind the shock wave is assumed isothermal rather than adiabatic to stimulate the conditions of large radiative transfer near the stellar surface. The product solution of McVittie has been used to obtain exact solution of the problem. It has been obtained that velocity, density, pressure and magnetic field increases as we move from shock surface towards the nucleus of the star.

Keywords

Magnetic Field Shock Wave Exact Solution Radiative Transfer Field Increase 

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References

  1. Bhatnagar, P. L. and Sachdev, P. L.: 1966,Nuovo Cimento 44, 15.Google Scholar
  2. Laumbach, D. D. and Probstein, R. F.: 1970,Phys. Fluids 13, 1178.Google Scholar
  3. McVittie, G. C.: 1953,Proc. Roy. Soc. London,A 220, 339.Google Scholar
  4. Pai, S. I.: 1958,Proc. Theor. Appl. Mech. 89, 000.Google Scholar
  5. Rogers, M. H.: 1957,Arch. Rational Mech. Anal. 1, 22.Google Scholar
  6. Rosenau, P. and Frankenthal, S.: 1976,Phys. Fluids 19, 1889.Google Scholar
  7. Sakurai, A.: 1960,Commun. Pure Applied Math. 13, 353.Google Scholar
  8. Whitham, G. B.: 1958,J. Fluid Mech. 4, 337.Google Scholar
  9. Zel'dovich, Ya. B. and Raizer, Yu. P.: 1967,Physics of Shock Waves and High-Temperature Hydrodynamic Phenomena, Academic Press, New York, Vol. II, Chapter XII.Google Scholar

Copyright information

© D. Reidel Publishing Co 1983

Authors and Affiliations

  • R. C. Srivastava
    • 1
  1. 1.Department of MathematicsGorakhpur UniversityGorakhpurIndia

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