Dynamical modeling and the interactions with the ISM

TL;DR

This review discusses recent advances in modeling planetary nebulae, their interactions with the interstellar medium, and the development of new observational and 3D morpho-kinematic techniques that enhance understanding of their structure and evolution.

Contribution

It introduces new formation mechanisms for multi-polar planetary nebulae based on binary interactions and instabilities, and summarizes progress in 3D modeling and ISM interaction simulations.

Findings

Progress in 3D morpho-kinematic modeling improves data interpretation.

Discovery of PNe showing clear signs of ISM interaction.

Hydrodynamic models explain observed nebula structures and predict IR signatures.

Abstract

This paper is a review of some of the recent modeling efforts to improve our understanding of structure formation and evolution of planetary nebulae including their interaction with the interstellar medium. New propositions have been made for the formation mechanism of multi-polar PNe and PPNe. These mechanisms are based on the central engine with interacting binary stars or hole producing instabilities in expanding shock waves leading to illumination effects from the central star that change the appearance of the nebula. Furthermore, there has been a lot of progress in the observation and 3D modeling of the kinematics, which is key to the understanding of the dynamics. Extensive observational catalogs are coming online for the kinematics, as well as some very detailed proper motion measurements have been made. New techniques for morpho--kinematic 3D modeling help to make the interpretation of kinematic data more reliable and detailed. In addition to individual pointed observations, new surveys have lead to the discovery of many PNe that show clear signs of interaction with the interstellar medium. Systematic hydrodynamic models of the interaction have produced a general scheme for the observed structure that results from the interaction of an evolving planetary nebula with the ISM. Detailed modeling of the dust-gas dynamics during the interaction with the ISM have produced interesting predictions for future IR observations. Detailed models were worked out for the structure of the bowshock and tail of Mira that was recently discovered in the UV.