Variability in Proto-Planetary Nebulae: I. Light Curve Studies of 12 Carbon-Rich Objects

TL;DR

This study presents a 14-year photometric monitoring of 12 carbon-rich proto-planetary nebulae, revealing complex pulsation behaviors, relationships between pulsation period, amplitude, and temperature, and implications for post-AGB evolution models.

Contribution

It provides long-term observational data showing pulsation period variations and challenges existing models linking pulsation to mass loss in post-AGB stars.

Findings

Inverse relationship between pulsation period and temperature.

Inverse relationship between amplitude and temperature.

Detection of long pulsation periods up to 150 days.

Abstract

We have carried out long-term (14 years) V and R photometric monitoring of 12 carbon-rich proto-planetary nebulae. The light and color curves display variability in all of them. The light curves are complex and suggest multiple periods, changing periods, and/or changing amplitudes, which are attributed to pulsation. A dominant period has been determined for each and found to be in the range of ~150 d for the coolest (G8) to 35-40 d for the warmest (F3). A clear, linear inverse relationship has been found in the sample between the pulsation period and the effective temperature and also an inverse linear relationship between the amplitude of light variation and the effective temperature. These are consistent with the expectation for a pulsating post-AGB star evolving toward higher temperature at constant luminosity. The published spectral energy distributions and mid-infrared images show these objects to have cool (200 K), detached dust shells and published models imply that intensive mass loss ended a few thousand years ago. The detection of periods as long as 150 d in these requires a revision in the published post-AGB evolution models that couple the pulsation period to the mass loss rate and that assume that intensive mass loss ended when the pulsation period had decreased to 100 d. This revision will have the effect of extending the time scale for the early phases of post-AGB evolution. It appears that real time evolution in the pulsation periods of individual objects may be detectable on the time scale of two decades.