The exotic helium variable PG 1346 + 082

Details The exotic helium variable PG 1346 + 082 The exotic helium variable PG 1346 + 082

Feb 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...313..757w&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 313, Feb. 15, 1987, p. 757-771. Research supported by the Council of Scient

Astronomy and Astrophysics

Astronomy

55

Astronomical Photometry, Binary Stars, Helium, Variable Stars, White Dwarf Stars, Absorption Spectra, Color-Magnitude Diagram, Light Curve, Spectral Line Width, Stellar Spectrophotometry, Ultraviolet Astronomy

Scientific paper

The results of an extensive study of the blue object PG 1346 + 082, which is both a photometric and a spectroscopic variable, are presented. The system spans the B magnitude range 13.6-17.2, is brighter than m(pg) of about 14.0 roughly 74 percent of the time, and has a photometric quasi-period of four to five days. The rapid photometric flickering at minimum light is identified as the signature of mass transfer in a binary sytsem, and the He I emission at minimum light as indicating the presence of an accretion disk. The inability to detect high-energy X-rays, the absence of the high-excitation lines of He II in the optical spectrum, and the complete absence of hydrogen in the spectrum show that PG 1346 + 082 is an interacting binary white dwarf system. This identification lends strong support to the interacting twin-degenerate interpretation for AM CVn. The outbursts of the system may be similar in physical origin to dwarf novae outbursts.

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