Detecting Planets in Planetary Nebulae

Abstract

We examine the possibility of detecting signatures of surviving Uranus-Neptune-like planets inside planetary nebulae. Planets that are not too close to the stars, orbital separation larger than about 5 AU, are likely to survive the entire evolution of the star. As the star turns into a planetary nebula, it has a fast wind and a strong ionizing radiation. The interaction of the radiation and wind with a planet may lead to the formation of a compact condensation or tail inside the planetary nebula, which emits strongly in Halpha, but not in [OIII]. The position of the condensation (or tail) will change over a time of about 10 years. Such condensations might be detected with currently existing telescopes.