Astronomy and Astrophysics – Astronomy
Scientific paper
Mar 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996apj...459..249r&link_type=abstract
Astrophysical Journal v.459, p.249
Astronomy and Astrophysics
Astronomy
16
Stars: Binaries: Eclipsing, Stars: Circumstellar Matter, Line: Profiles, Stars: Individual Constellation Name: Beta Persei
Scientific paper
The Hα difference profiles of fl Per obtained from 1976 to 1977 have been analyzed in several ways to study the gas flows in the binary. These difference profiles were obtained by removing the combined stellar photospheric absorption contribution from the observed profiles to enhance the weak emission from circumstellar gas. The difference profiles display strong narrow single-peaked emission and broader double-peaked emission. The line strengths peaked near phase 0.7 for the blueshifted emission and near phase 0.2 for the redshifted emission. These maxirna occur at phases where our line of sight would pass through the gas stream or an accretion region located between the stars. The orbital variations of the radial velocities of the single- and double-peaked emission followed S-waves. The source of the single- peaked emission was found at velocities close to the L_{1 }point on the side of the secondary star in the direction of the gas stream trajectory, as if associated with the gas stream. However, the source of the double-peaked emission was found at velocities almost halfway between that of the stars, in the direction away from the gas stream. The double-peaked nature of these profiles imply that they arise from an accretion region surrounding the primary star, with the most intense, concentrated part between the stars. Reconstructed Doppler images of the binary from Doppler tomography are consistent with the S-wave analysis and show that there are several sources of emission (from strongest to weakest): a gas stream, a localized region, and an unstable asymmetric accretion annulus. The gas stream extends from the L_{1 }point to the impact site on the stellar surface, but it tapers sharply about halfway along its path as if blocked by material around the primary. Finally, the weakest source arose from the region around the secondary star, so chromospheric emission from the magnetically active subgiant secondary has been detected in the Doppler image.
Jones Robert D.
Richards Mercedes T.
Swain Melanie A.
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