Roche Tomography of the Cool Star in IP Peg
We analyse orbitally-resolved spectra of the Na i doublet in the dwarf nova IP Peg, using the newly developed technique of Roche tomography. We show that Roche tomography can be successfully employed to image the secondary stars in CVs, and that it also serves as an independent aid for determining binary system parameters. Our preliminary results suggest that the mass of the white-dwarf primary is 1.2 M⊙, significantly higher than previous estimates.
KeywordsRadial Velocity Binary Star Line Strength Stellar Surface Orbital Phase
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- Martin, J.S., Jones, D.H.P., Smith, R.C., 1987, MNRAS, 224, 1031Google Scholar