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PG1159-035: A New, Hot, Non-DA Pulsating Degenerate

Published online by Cambridge University Press:  12 April 2016

J. T. McGraw ,
S. G. Starrfield ,
J. Liebert  and
R. Green
J. T. McGraw
Affiliation:
Steward Observatory, University of Arizona
S. G. Starrfield*
Affiliation:
Steward Observatory, University of Arizona
J. Liebert
Affiliation:
Steward Observatory, University of Arizona
R. Green
Affiliation:
Department of Astronomy, California Institute of Technology
*
* Permanent address, Dept. of Physics, Arizona State University; present address, Theoretical Division, Los Alamos Scientific Laboratory

Extract

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PG1159-035 was originally detected as a 14.5 mag. blue object in a survey for QSO candidates (Green 1977), An SIT spectrogram obtained at the Hale 5m telescope at 6Å resolution showed this star to have a very blue continuum with absorption features near λ4686 and λ4650 which were tentatively attributed to Hell and the CIII/CIV complex, respectively. Possible narrow emission components to these lines appear in Figure 1 which shows confirming spectra obtained with the IIDS (at 2.5Å resolution) on the Kitt Peak 2.1m telescope. The blue continuum and possible presence of Hell in emission suggested that this star was perhaps similar to the helium mass-transfer binary AM CVn (HZ 29). For this reason, we put PG1159-035 on our program of high-speed photometry, expecting the star to show “flickering” associated with mass transfer into an accretion disk and possible orbital modulation or eclipses in the period range 10-20 minutes—photometric characteristics similar to those observed in AM CVn.

Type
Colloquium Session VI
Information
International Astronomical Union Colloquium , Volume 53: White Dwarfs and Variable Degenerate Stars , August 1979 , pp. 377 - 381
Copyright
Copyright © The University of Rochester 1979

References

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