Defining the instability strip of pulsating post-AGB binary stars from ASAS and NSVS photometry

Details Defining the instability strip of pulsating post-AGB binary stars from ASAS and NSVS photometry Defining the instability strip of pulsating post-AGB binary stars from ASAS and NSVS photometry

2006-12-08

arxiv.org/abs/astro-ph/0612217v1

Mon.Not.Roy.Astron.Soc.375:1338-1348,2007

Astronomy and Astrophysics

Astrophysics

11 pages & 9 figures, accepted for publication in MNRAS (Dec. 8)

Scientific paper

10.1111/j.1365-2966.2006.11387.x

We analyse public domain time-series photometric observations of 30 known and candidate binary post-AGB stars for measuring pulsation and orbital periods. We derive periodicities for 17 stars for the first time in the literature. Besides identifying five new RV Tauri type pulsating variables (three with the RVb phenomenon, i.e. long-term changes of the mean brightness), we find multiply periodic (or possibly irregular) post-AGB stars on the two edges of the instability strip. The temperature dependence of the peak-to-peak light curve amplitudes clearly indicates the changes in excitation as post-AGB stars evolve through the strip. One object, the peculiar Type II Cepheid ST Pup, showed a period increase from 18.5 to 19.2 d, which is consistent with the known period fluctuations in the past. In HD 44179, the central star of the Red Rectangle nebula, we see very similar asymmetric light curve than was measured 10-15 years ago, suggesting a very stable circumstellar environment. In contrast to this, HD 213985 shows coherent but highly non-repetitive brightness modulation, indicating changes in the circumstellar cloud on a similar time-scale to the orbital period.

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