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Gravitational Redshifts for Hyades White Dwarfs*

Published online by Cambridge University Press:  12 April 2016

G. Wegner ,
I. N. Reid  and
R. K. McMahan
G. Wegner
Affiliation:
Department of Physics & Astronomy, Dartmouth College
I. N. Reid
Affiliation:
California Institute of Technology
R. K. McMahan
Affiliation:
Harvard-Smithsonian Center for Astrophysics

Extract

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Precise white dwarf gravitational redshifts can only be obtained utilizing systems of known distance and space velocity. Binaries with known orbits such as 40 Eri B are rare, and although common proper motion pairs have proven highly useful(Wegner 1973: Koester 1987: Wegner & Reid 1987), there are some problems in their interpretation. Another approach is to employ white dwarfs in open clusters; they not only have known systemic velocities, but also provide information on the progenitors of the white dwarfs. Of the nearby galactic clusters, the Hyades currently give the best information for achieving accurate gravitational redshifts: the members are relatively bright and nearby and their kinematics are well known.

Type
Research Article
Information
International Astronomical Union Colloquium , Volume 114: White Dwarfs , 1989 , pp. 378 - 383
Copyright
Copyright © Springer-Verlag 1989

Footnotes

*

Some of the spectroscopic observations were obtained at the Multiple Mirror Telescope Observatory, a joint facility of the University of Arizona and the Smithsonian Institution.

References

Cameron, L.M. 1985, Astron. & Astrophys., 152, 250.Google Scholar
Grabowski, B., Madej, J. & Halenka, J. 1987, Astrophys. J., 313, 750.CrossRefGoogle Scholar
Greenstein, J.L. 1974, Astrophys. J. (Letters). 189, L131.Google Scholar
Greenstein, J.L., Boksenberg, A. Carswell, R., & Shortridge, K. 1977, Astrophys. J., 212, 186.Google Scholar
Greenstein, J.L. and Peterson, D.M. 1973, Astron. & Astrophys., 25, 29.Google Scholar
Greenstein, J.L. and Trimble, V.L. 1967, Astrophys. J., 149, 283.Google Scholar
Hamada, T. & Salpeter, E.E. 1961, Astrophys. J., 134, 683.CrossRefGoogle Scholar
Hanson, R. 1980, in Star Clusters, IAU Colloq. No. 85. Hesser, J.E., ed., (Dordrecht: Reidel), p. 71.Google Scholar
Hanson, R. & Vasilevskis, S. 1983. Astron. J., 88, 844.CrossRefGoogle Scholar
Luyten, W.J. 1971, The Hyades, (Minneapolis: Univ. Minnesota).Google Scholar
Koester, D. 1987, Astrophys. J., 322, 852.Google Scholar
Koester, D. & Schönberner, D. 1986, Astron. & Astrophys., 154, 125.Google Scholar
McCook, G.P. & Sion, E.P. 1987, Astrophys. J. Suppl. 65, 603.Google Scholar
McMahan, R.K. 1986, Ph.D. Thesis. Dartmouth College.Google Scholar
Oke, J.B., Weidemann, V. & Koester, D. 1984, Astrophys. J., 281, 276.Google Scholar
Peterson, D.M. & Smolensky, R. 1987, Astrophys. J., 315, 286.Google Scholar
Stefanik, R.P. and Latham, D.W. 1985. in Stellar Radial Velocities, Proc. IAU Colloq. No. 88, Philip, A.G.D. and Latham, D.W., eds., (Schenectady: L. Davis Press), p. 213.Google Scholar
Trimble, V. & Greenstein, J.L. 1972, Astrophys. J., 111, 441.Google Scholar
van Altena, W.F. 1969, Astron J., 14, 2.Google Scholar
Wegner, G. 1973. Mon. Not. R. astr. Soc. 165, 271.CrossRefGoogle Scholar
Wegner, G. 1980, Astron. J., 85, 1255 Google Scholar
Wegner, G. & McMahan, R.K. 1985, Astron. J., 90, 1511.CrossRefGoogle Scholar
Wegner, G. and Nelan, E.P. 1987, Astropys. J., 319, 916.Google Scholar
Wegner, G. and Reid, I.N. 1987. in The Second Conference on Faint Blue Stars, Proc. IAU Coloq. No. 95. Philip, A.G.D., Hayes, D.S., and Liebert, J.W.. eds., (Schenectady: L. Davis Press), p. 649. Google Scholar
Weidemann, V. & Koester, D. 1983. Astron. & Astrophys., 121, 77.Google Scholar