Astronomy and Astrophysics – Astronomy
Scientific paper
May 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...180.2701j&link_type=abstract
American Astronomical Society, 180th AAS Meeting, #27.01; Bulletin of the American Astronomical Society, Vol. 24, p.768
Astronomy and Astrophysics
Astronomy
4
Scientific paper
The Hα difference profiles of β Per contain several emission components (Richards 1992, ApJ, 387, 329): a relatively strong narrow single-peaked emission profile which was redshifted relative to the rest wavelength of the Hα line in the frame of the center of mass of the B8 V primary near phase 0.2 and blueshifted near phase 0.7; and a weaker double-peaked emission feature which was visible near secondary eclipse. The single-peaked emission is believed to be due to a high density localized region close to the expected position of the star-stream impact region or to the gas stream from the K2 IV secondary; while the double-peaked emission arises from a transient accretion disk around the B8 V primary. We have re-examined these emission profiles in terms of their Doppler shifts and emission line strengths in an attempt to more precisely determine the source of the single-peaked emission. The phase dependence of the radial velocities of the narrow emission peaks in the difference profiles is an S-wave, indicative of a spot or a gas stream. We used Doppler Tomography (Marsh and Horne 1988, MNRAS, 235, 269) to determine the source of the strong narrow emission profiles in the orbital plane of the binary, and found the Doppler image of the emitting region. The phase dependence of the emission line strengths was also used to isolate the source. The line strengths peaked near phase 0.7 for the blueshifted emission and near phase 0.2 for the redshifted emission. These maxima occur at phases where our line of sight would pass though the middle of the localized region. This result is encouraging since the localized region was found from the transition phases where emission changed to absorption and vice versa. This work was partially supported by NSF grant AST 91-14214 to MTR.
Jones Robbie D.
Richards Mercedes T.
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