Full-Orbit Hα Spectroscopy of Short-Period ALGOLS

Details Full-Orbit Hα Spectroscopy of Short-Period ALGOLS Full-Orbit Hα Spectroscopy of Short-Period ALGOLS

May 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...180.2707a&link_type=abstract

American Astronomical Society, 180th AAS Meeting, #27.07; Bulletin of the American Astronomical Society, Vol. 24, p.769

Astronomy and Astrophysics

Astronomy

2

Scientific paper

Hα CCD spectra of the short-period Algols TX UMa, RW Tau, and β Per were obtained with the stellar spectrograph on the 1.5m telescope at the McMath Solar Observatory, NOAO, during the night-time synoptic program from 1989 to 1992. These data are part of a long-term project to determine precise spatial information about the circumstellar material in these systems from spectra obtained over the entire orbit of the binary. At the present time the phase coverage of the orbits of these binaries is incomplete, but there is clear evidence of circumstellar material in each binary. All of the binaries observed show either redshifted or blueshifted emission above the wings of the uncontaminated Hα line profile, or excess absorption mostly in the line core. The 1991 observations of TX UMa (P = 3.0632 days) show evidence of redshifted emission in the wing of the Hα line profile which gradually increased in strength throughout the range of observations from phase 0.11 to 0.17, with peak strength at phase 0.16. The 1989 observations of RW Tau (P = 2.7688 days) were obtained at mean phases of 0.53 and 0.54. These profiles show evidence of weak double-peaked emission with the blueshifted peak stronger than the redshifted peak. Finally, the 1989 and 1990 observations of β Per (P = 2.8673 days) show evidence of blueshifted emission above the wings of the undisturbed profile between phases 0.81 and 0.82, similar redshifted emission between about half an orbit away which increased in strength between phases 0.16 and 0.21, and excess absorption from circumstellar material which increased in strength between phases 0.91 and 0.93. All of these short-period Algols display spectra which contain clear evidence of emission or excess absorption from circumstellar gas, and the phase dependence of the circumstellar features are very similar to that seen in earlier data of β Per by Richards (1992; ApJ, 387, 329). This work was partially supported by NSF grants AST 89-01238 and AST 91-14214 to MTR.

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