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• W2025594328 abstract "view Abstract Citations References Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Astrometric-Spectroscopic Triple System Mizar B. Beardsley, Wallace K. Abstract 68, 352, 1963) has yielded orbital residuals with a period of 3.7 yr and a semiamplitude of the same order as the parallax. H.A. Abt (Astrophys. J. Suppl. 6, 37,1961) found that another orbit existed and suggested a period of 1.0 yr. From new spectroscopic data obtained over the past three years at the Dominion Astrophysical Observatory F. Gutmann (Quart. J. Roy. Astron. Soc., 5, 40,1964) has found this period to be 0.5 yr. I have analyzed the monthly means of all published radial velocities. Successive approximations were used beginning with a guess as to what the 3. 7-yr radial velocity orbit might look like based on the astrometric results. Removal of this orbit from the monthly means gave independent confirmation to the 0.5-yr orbit. Continued approximation and removal of first one and then the other orbit over some 50 yr of observations has yielded fairly reliable radial velocity curves for these orbits. Apparent rapid fluctuation of the individual radial velocities also indicated the presence of a possible short-term periodicity. Removal of both long periods from the individual radial velocities indicated this variation to be less than 0.2 day. A series of eight spectrograms at the Allegheny Observatory on 26 April 1964 confirmed this and implied the variation is due to pulsation. A possible change in period and amplitude of this pulsation is being investigated. Preliminary orbital elements are: P1=1350days, e1=0.20, w1=2700, velocity range =8.8 km/sec, ~i = -8.0km/sec; P2 = 182.33 days, e2 =0.60, ~2 = 350~, velocity range =19.7 km/sec; P3 <0.2 days (pulsation). For the series on 26 April 1964 the pulsation was measured from the metallic lines. These lines generally yielded a significantly different velocity from the H, Ca II, Mg II, lines which evidently were blended by the other star in 0.5-yr system. These metallic lines also showed evidence of doubling at the positive peak of the variation. From this doubling it is possible to infer that the pulsating star is the Am star and is slightly more massive than the other star in the 0.5-yr system (probably early F) while about these two stars revolves another star (probably early G) in a 3. 7-yr orbit. Definitive orbits are being determined at Allegheny Observatory utilizing both astrometric and spectroscopic data. Publication: The Astronomical Journal Pub Date: 1964 DOI: 10.1086/109438 Bibcode: 1964AJ.....69R.532B full text sources ADS |" @default.
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• W2025594328 date "1964-01-01" @default.
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• W2025594328 title "Astrometric-Spectroscopic Triple System Mizar B." @default.
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