Other
Scientific paper
Jan 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984aj.....89..119h&link_type=abstract
Astronomical Journal (ISSN 0004-6256), vol. 89, Jan. 1984, p. 119-125. Research supported by the Natural Sciences and Engineerin
Other
22
Abundance, Binary Stars, Cepheid Variables, Stellar Evolution, Stellar Motions, Stellar Temperature, Metallicity, Orbital Elements, Peculiar Stars, Radial Velocity, Stellar Oscillations, Stellar Spectrophotometry
Scientific paper
Continued spectroscopy of AU Peg, a peculiar Type II Cepheid, has allowed determination of the orbital period, separation of the pulsation and orbital velocities, and solution of the single-line binary orbit. The companion is probably more massive than AU Peg, and is probably a compact object. It is sufficiently close that mass transfer must have occurred within the system in the past. A high dispersion abundance analysis shows that AU Peg has Fe/H = +0.1, and is considerably cooler than normal for its period. AU Peg is outside the normal instability strip, lying approximately 500 K cooler than the normal red edge. One possible explanation, a high helium abundance, is discussed. The large period increase remains to be explained. Interactions with binary companions may be important for other Type II Cepheids.
Harris Hugh C.
Olszewski Edward W.
Wallerstein George
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