Hostname: page-component-cd9895bd7-dzt6s Total loading time: 0 Render date: 2024-12-26T04:16:14.716Z Has data issue: false hasContentIssue false
  • English
  • Français

Wave propagation in the magnetized cores of white dwarf stars with ultra-relativistic degenerate electrons

Published online by Cambridge University Press:  10 May 2011

P. K. SHUKLA ,
D. A. MENDIS  and
S. I. KRASHENINNIKOV
P. K. SHUKLA
Affiliation:
International Centre for Advanced Studies in Physical Sciences, Institute for Theoretical Physics, Faculty of Physics and Astronomy, Ruhr University Bochum, 44780 Bochum, Germany (ps@tp4.ruhr-uni-bochum.de)
D. A. MENDIS
Affiliation:
Jacobs School of Engineering, University of California, San Diego, La Jolla, CA 92093, USA
S. I. KRASHENINNIKOV
Affiliation:
Jacobs School of Engineering, University of California, San Diego, La Jolla, CA 92093, USA
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We discuss the dispersive properties of low-frequency electromagnetic (EM) perturbations in the magnetized core of self-gravitating white dwarf stars with ultra-relativistic degenerate electrons. For our purposes, we derive a dispersion relation by using the hydrodynamic equations for the ions under the action of EM and self-gravitating forces, and the inertialess electrons under the action of EM forces and the gradient of the ultra-relativistic pressure. The dispersion relation admits stability of a white dwarf star against a class of EM perturbations whose wavelengths are shorter than 15000 km.

Type
Letter
Information
Journal of Plasma Physics , Volume 77 , Issue 5 , October 2011 , pp. 571 - 575
Copyright
Copyright © Cambridge University Press 2011.

References

[1]Shapiro, S. L. and Teukolsky, S. L. 1983 Black Holes, White Dwarfs, and Neutron Stars: The Physics of Compact Objects. New York: John Wiley & Sons.CrossRefGoogle Scholar
[2]Chandrasekhar, S. 1931 Phil. Mag. 11, 591.CrossRefGoogle Scholar
[3]Chandrasekhar, S. 1931 Astrophys. J. 74, 81.CrossRefGoogle Scholar
[4]Chandrasekhar, S. 1935 Mon. Not. R. Astron. Soc. 170, 405.Google Scholar
[5]Chandrasekhar, S. 1939 An Introduction to the Study of Stellar Structure. Dover Publications, pp. 412.Google Scholar
[6]Libert, J. 1980 Ann. Rev. Astron. Astrophys. 18, 363.CrossRefGoogle Scholar
[7]Gatewood, G. D. and Gatewood, C. V. 1978 Astrophys. J. 225, 191.CrossRefGoogle Scholar
[8]Chandrasekhar, S. 1964 Phys. Rev. Lett. 12, 114.CrossRefGoogle Scholar
[9]Chandrasekhar, S. and Tooper, R. F. 1964 Astrophys. J. 139, 1396.CrossRefGoogle Scholar
[10]Avinash, K. and Shukla, P. K. 1994 Phys. Lett. A 189, 470.CrossRefGoogle Scholar
[11]Shukla, P. K. and Stenflo, L. 2006 Phys. Lett. A 355, 378.CrossRefGoogle Scholar