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Doppler Tomography

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Astrotomography

Part of the book series: Lecture Notes in Physics ((LNP,volume 573))

Abstract

I review the method of Doppler tomography which translates binary-star line profiles taken at a series of orbital phases into a distribution of emission over the binary. I begin with a discussion of the basic principles behind Doppler tomography, including a comparison of the relative merits of maximum entropy regularisation versus filtered back-projection for implementing the inversion. Following this I discuss the issue of noise in Doppler images and possible methods for coping with it. Then I move on to look at the results of Doppler Tomography applied to cataclysmic variable stars. Outstanding successes to date are the discovery of two-arm spiral shocks in cataclysmic variable accretion discs and the probing of the stream/magnetospheric interaction in magnetic cataclysmic variable stars. Doppler tomography has also told us much about the stream/disc interaction in non-magnetic systems and the irradiation of the secondary star in all systems. The latter indirectly reveals such effects as shadowing by the accretion disc or stream. I discuss all of these and finish with some musings on possible future directions for the method. At the end I include a tabulation of Doppler maps published in refereed journals.

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Author information

Authors and Affiliations

  1. Department of Physics and Astronomy, Southampton University, Highfield, SO17 1BJ, Southampton

    T.R. Marsh

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  1. T.R. Marsh
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Editors and Affiliations

  1. Royal Observatory of Belgium, Avenue Circulaire, 3, 1180, Brussels, Belgium

    Henri M.J. Boffin  & Jan Cuypers  & 

  2. Department of Physics and Astronomy, University of Southampton, Highfield, SO17 1BJ, Southampton, UK

    Danny Steeghs

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Marsh, T. (2001). Doppler Tomography. In: Boffin, H.M., Cuypers, J., Steeghs, D. (eds) Astrotomography. Lecture Notes in Physics, vol 573. Springer, Berlin, Heidelberg. https://doi.org/10.1007/3-540-45339-3_1

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  • DOI: https://doi.org/10.1007/3-540-45339-3_1

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