RECORD
Doppler Tomography
Astrophysics · Submitted 1 Nov 2000
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim 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.
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The abstract, sentence by sentence
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.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | 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. | method 0.44 | 0.16 | 0.10 | asserted 0.99 |
| s1 | 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. | method 0.62 | 0.22 | 0.03 | asserted 0.74 |
| s2 | Following this I discuss the issue of noise in Doppler images and possible methods for coping with it. | method 0.59 | 0.13 | 0.02 | unclear 0.57 |
| s3 | Then I move on to look at the results of Doppler Tomography applied to cataclysmic variable stars. | contribution 0.75 | 0.21 | 0.04 | asserted 0.67 |
| s4 | 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. | result 0.90 | 0.15 | 0.28 | asserted 1.00 |
| s5 | 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. | result 0.86 | 0.16 | 0.14 | asserted 1.00 |
| s6 | The latter indirectly reveals such effects as shadowing by the accretion disc or stream. | interpretation 0.90 | 0.10 | 0.05 | asserted 0.95 |
| s7 | I discuss all of these and finish with some musings on possible future directions for the method. | future work 0.89 | 0.53 | 0.05 | unclear 0.40 |
| s8 | At the end I include a tabulation of Doppler maps published in refereed journals. | contribution 0.92 | 0.69 | 0.02 | asserted 0.93 |
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Original 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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