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Accretion Flow along a Dipolar Field: Application to Intermediate Polars

Published online by Cambridge University Press:  12 April 2016

João Batista Garcia Canalle ,
Kinwah Wu ,
Mark Cropper ,
Gavin Ramsay  and
Curtis J. Saxton
João Batista Garcia Canalle
Affiliation:
Physics Institute, State University of Rio de Janeiro, Rua São Francisco Xavier, 524/3023-D, CEP 20559-900, Rio de Janeiro, RJ, Braziland Mullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking, Surrey RH5 6NT, United Kingdom
Kinwah Wu
Affiliation:
Mullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking, Surrey RH5 6NT, United Kingdom
Mark Cropper
Affiliation:
Mullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking, Surrey RH5 6NT, United Kingdom
Gavin Ramsay
Affiliation:
Mullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking, Surrey RH5 6NT, United Kingdom
Curtis J. Saxton
Affiliation:
Mount Stromlo and Siding Spring Observatory, Research School of Astronomy and Astrophysics, Australian National University, ACT 0200, Australia

Abstract

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A hydrodynamic formulation for accretion flow channeled by a dipolar magnetic field is constructed using a curvi-linear coordinate system natural to the field structure. We solve the hydrodynamic equations and determine the velocity, density and temperature profiles of the post-shock accretion flow. The results are applied to accretion flows in intermediate polars. We have found that for systems with massive white dwarfs (~ 1 M⊙) the temperature profiles in the flow can differ significantly to those obtained from models in which the accretion column is assumed to be cylindrical.

Type
Part 3. B. Accretion Plasma diagnostics - Theory
Information
International Astronomical Union Colloquium , Volume 190: Magnetic Cataclysmic Variables , 2004 , pp. 208 - 214
Copyright
Copyright © Astronomical Society of the Pacific 2004

References

Aizu, k. 1973, Prog. Theor. Phys., 49, 1184 CrossRefGoogle Scholar
Canalle, J. B. G., et al. 2003, MNRAS, to be submittedGoogle Scholar
Chevalier, R. A., & Imamura, J. N. 1982, ApJ, 261, 543 CrossRefGoogle Scholar
Cropper, M., Ramsay, G., & Wu, k. 1998, MNRAS, 293, 222 CrossRefGoogle Scholar
Cropper, M., Wu, K., Ramsay, G., & Kocabiyik, A. 1999, MNRAS, 306, 684 CrossRefGoogle Scholar
Cropper, M., Ramsay, G., Hellier, C., Mukai, K., Mauche, C., & Pandel, D., 2002, Trans. Phil. Trans. R. Soc. Lon. A, 360, 1951 Google Scholar
Lamb, D. Q., & Masters, A. R. 1979, ApJ, 234, L117 Google Scholar
Nauenberg, M. 1972, ApJ, 175, 417 CrossRefGoogle Scholar
Ramsay, G., 2000, MNRAS, 314, 403 Google Scholar
Wickramasinghe, D. T., & Meggitt, S. M. A. 1985, MNRAS, 214, 605 Google Scholar
Wu, K. 1994, Proc. Astron. Soc. Australia, 11, 61 Google Scholar
Wu, K. 2000, Space Sci. Rev., 93, 611 Google Scholar
Wu, K., Chanmugam, G., & Shaviv, G. 1994, ApJ, 426, 664 Google Scholar