Document Type
Article
Publication Date
9-1-2005
Abstract
We report a photometric study of the WZ Sagittae-type dwarf nova PQ Andromedae. The light curve shows strong (0.05 mag full amplitude) signals with periods of 1263(1) and 634(1) s, and a likely double-humped signal with P = 80.6(2) minutes. We interpret the first two as nonradial pulsation periods of the underlying white dwarf, and the last as the orbital period of the underlying binary. We estimate a distance of 150(50) pc from proper motions and the two standard candles available: the white dwarf and the dwarf-nova outburst. At this distance, the K magnitude implies that the secondary is probably fainter than any star on the main sequence-indicating a mass below the Kumar limit at 0.075 M⊙. PQ And may be another "period bouncer," where evolution now drives the binary out to a longer period. © 2005. The Astronomical Society of the Pacific. All rights reserved.
Publication Source (Journal or Book title)
Publications of the Astronomical Society of the Pacific
First Page
922
Last Page
927
Recommended Citation
Patterson, J., Thorstensen, J., Armstrong, E., Henden, A., & Hynes, R. (2005). The dwarf nova PQ andromedae. Publications of the Astronomical Society of the Pacific, 117 (835), 922-927. https://doi.org/10.1086/432492