Titlebook: Astrotomography; Indirect Imaging Met Henri M.J. Boffin,Jan Cuypers,Danny Steeghs Book 2001 Springer-Verlag Berlin Heidelberg 2001 Accretio

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書目名稱Astrotomography影響因子(影響力)




書目名稱Astrotomography影響因子(影響力)學(xué)科排名




書目名稱Astrotomography網(wǎng)絡(luò)公開度




書目名稱Astrotomography網(wǎng)絡(luò)公開度學(xué)科排名




書目名稱Astrotomography被引頻次




書目名稱Astrotomography被引頻次學(xué)科排名




書目名稱Astrotomography年度引用




書目名稱Astrotomography年度引用學(xué)科排名




書目名稱Astrotomography讀者反饋




書目名稱Astrotomography讀者反饋學(xué)科排名

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Foundation iPhone App Developments 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 pub

thwart

Jordan Hamson-Utley,Errin Heymanthe Doppler tomography technique that relaxes one of the basic assumptions of tomography, and is able to map modulated emission sources. This extension allows us to fit anisotropic emission from, for example, spirals shocks, the irradiated companion star and disc-stream interaction sites.

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Foundation iPhone App Developmenton 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 imag

Concerto

David Gibson,Kathryn Coleman,Leah Irvingobserved in previous UV and optical data. We find that the central spike contributes to the flare spectra indicating that its origin is probably the compact object. We also detect that the central spike moves with orbital phase following an S-wave pattern. The radial velocity semiamplitude of the S-

esoteric

Melinda J. Lewis,Jason M. Lodgeuring our observations. All of them have visible mass donor stars allowing us to establish precise orbital phases. None of them show what is often thought of as the classic pattern of symmetric disc plus bright-spot at the gas stream/disc impact. Instead they have regions of emission at low velociti

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Jordan Hamson-Utley,Errin Heymano resolve and map such co-rotating patterns and allows a straightforward comparison with theory. The dwarf nova IP Pegasi presents the best studied case, carrying two spiral arms in a wide range of emission lines throughout its outbursts. Both arms appear at the locations where tidally driven spiral

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