Interaction of planetary nebulae, Eta-Carinae and supernova remnants with the Interstellar Medium

TL;DR

This paper develops a comprehensive model of planetary nebulae, Eta-Carinae, and supernova remnants interacting with the interstellar medium, incorporating shell expansion, particle diffusion, and line-of-sight imaging, validated against observed data.

Contribution

It introduces a unified framework combining shell dynamics, particle diffusion, and image synthesis for diverse astrophysical objects, with detailed comparisons to observations.

Findings

Successful modeling of nebulae and remnants with observed intensity profiles

Analysis of diffusion processes in different geometries and conditions

Validation of theoretical models against real astronomical data

Abstract

The image of planetary nebulae (PN), supernova remnant (SNR) and Eta-Carinae is made by three different physical processes. The first process is the expansion of the shell that can be modeled by the canonical laws of motion in the spherical case and by the momentum conservation when gradients of density are present in the interstellar medium. The quality of the simulations is introduced along one direction as well along many directions. The second process is the diffusion of particles that radiate from the advancing layer. The 3D diffusion from a sphere, the 1D diffusion with drift and 1D random walk are analyzed. The third process is the composition of the image through an integral operation along the line of sight. The developed framework is applied to three PN which are A39, the Ring nebula and the etched hourglass nebula MyCn 18, the hybrid object Eta-Carinae, and to two SNR which are SN 1993J and SN 1006. In all the considered cases a careful comparison between the observed and theoretical profiles in intensity is done.