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The Time Dependence of the Phases of the Harmonics Relative to the 1490 sec Fundamental in PG1346+082

Published online by Cambridge University Press:  12 April 2016

J. L. Provencal ,
J. C. Clemens ,
G. Henry ,
B. P. Hine ,
R. E. Nather ,
D. E. Winget ,
M. A. Wood ,
S. O. Kepler ,
G. Vauclair  and
M. Chevreton
...Show all authors
J. L. Provencal
Affiliation:
McDonald Observatory and Department of Astronomy, The University of Texasat AustinU.S.A.
J. C. Clemens
Affiliation:
McDonald Observatory and Department of Astronomy, The University of Texasat AustinU.S.A.
G. Henry
Affiliation:
McDonald Observatory and Department of Astronomy, The University of Texasat AustinU.S.A.
B. P. Hine
Affiliation:
McDonald Observatory and Department of Astronomy, The University of Texasat AustinU.S.A.
R. E. Nather
Affiliation:
McDonald Observatory and Department of Astronomy, The University of Texasat AustinU.S.A.
D. E. Winget
Affiliation:
McDonald Observatory and Department of Astronomy, The University of Texasat AustinU.S.A.
M. A. Wood
Affiliation:
McDonald Observatory and Department of Astronomy, The University of Texasat AustinU.S.A.
S. O. Kepler
Affiliation:
Instituto de Fisica, Universidade Federal do Rio Grande do Sul, Brazil
G. Vauclair
Affiliation:
Observatoire Midi-Pyrenees et Observatoire de MeudonFrance
M. Chevreton
Affiliation:
Observatoire Midi-Pyrenees et Observatoire de MeudonFrance
D. O’Donoghue
Affiliation:
Department of AstronomyUniversity of Cape Town, South Africa
B. Warner
Affiliation:
Department of AstronomyUniversity of Cape Town, South Africa
A. D. Grauer
Affiliation:
University of Arkansasat Little RockU.S.A.
Lilia Ferrario
Affiliation:
Australian National University, Australia

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White dwarf stars provide important boundary conditions for the understanding of stellar evolution. An adequate understanding of even these simple stars is impossible without detailed knowledge of their interiors. PG1346+082, an interacting binary white dwarf system, provides a unique opportunity to view the interior of one degenerate as it is brought to light in the accretion disk of the second star as the primary strips material from its less massive companion (see Wood et at. 1987).

PG1346+082 is a photometric variable with a four magnitude variation over a four to five day quasi-period. A fast Fourier transform (FFT) of the light curve shows a complex, time-dependent structure of harmonics. PG1346+082 exhibits flickering – the signature of mass transfer. The optical spectra of the system contain weak emission features during minimum and broad absorption at all other times. This could be attributed to pressure broadening in the atmosphere of a compact object, or to a combination of pressure broadening and doppler broadening in a disk surrounding the compact accretor. No hydrogen lines are observed and the spectra are dominated by neutral helium. The spectra also display variable asymmetric line profiles.

Type
Research Article
Information
International Astronomical Union Colloquium , Volume 114: White Dwarfs , 1989 , pp. 296 - 299
Copyright
Copyright © Springer-Verlag 1989

References

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