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The Orbital Period of G61-29

Published online by Cambridge University Press:  12 April 2016

R. E. Nather ,
E. L. Robinson  and
R. J. Stover
R. E. Nather
Affiliation:
McDonald Observatory and Department of Astronomy, University of Texas at Austin
E. L. Robinson
Affiliation:
McDonald Observatory and Department of Astronomy, University of Texas at Austin
R. J. Stover
Affiliation:
McDonald Observatory and Department of Astronomy, University of Texas at Austin

Extract

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The proper-motion star G61-29 (Giclas et al 1971) was discovered to have an emission-line spectrum consisting entirely of helium by Burbidge and Strittmatter (1971), who noted that the very broad lines (ca. 32 Å at λ4471) seemed to have variable profiles. Warner (1972) suggested that the star might be a close binary system, with the emission lines arising from an accretion disk surrounding a white dwarf, and searched for evidence of binary motion using high speed photometry. He suggested a tentative orbital period of 6h 16m, which subsequent observations were unable to confirm. Smak (1975) studied the star spectroscopically and agreed with Warner’s accretion disk hypothesis based on his analysis of the emission line profiles, but was also unable to derive evidence of orbital motion from his spectra, which were exposed for about 40 minutes each. Greenstein et al.(1977) also observed profile variations in spectra with shorter exposures, but evidently did not search for periodicities.

Type
Colloquium Session VII
Information
International Astronomical Union Colloquium , Volume 53: White Dwarfs and Variable Degenerate Stars , August 1979 , pp. 453 - 457
Copyright
Copyright © The University of Rochester 1979

References

Bopp, B.W., Evans, D.S., Laing, J.D. and Deeming, T.J. 1970, M.N.R.A.S. 147, 355.Google Scholar
Burbidge, E.M. and Strittmatter, P.A. 1971, Ap.J. 170, L39.Google Scholar
Faulkner, J., Flannery, B.P. and Warner, B. 1972, Ap.J. 175, L79.Google Scholar
Giclas, H.L., Burnham, R. and Thomas, N.G. 1971, Lowell Proper Motion Survey (Lowell Observatory, Flagstaff, AZ).Google Scholar
Greenstein, J.L., Arp, H.C. and Shectman, S. 1977, P.A.S.P. 89, 741.CrossRefGoogle Scholar
Shavlv, G. and Kovetz, A. 1976, A. and A. 51, 383.Google Scholar
Kraft, R.P. 1963, Adv. Astron. Astrophys. 2, 43.Google Scholar
Patterson, J., Nather, R.E., Robinson, E.L. and Handler, F. 1979, Ap.J. 232, (in press).Google Scholar
Robinson, E.L. and Faulkner, J. 1975, Ap.J. 200, L23.Google Scholar
Smak, J.I. 1975, Acta Astronomica 25, 227.Google Scholar
Tull, R.G., Vogt, S.S. and Kelton, P.W. 1979, Proc. S.P.I.E. 172.Google Scholar
Warner, B. 1972, M.N.R.A.S. 159, 315.Google Scholar