Pa 30 : study on a possible origin of its peculiar morphology

In Astrophysics modern era, as well as in all natural sciences, computers are used to perform simulations, the main complementary tool to observations, simulations play a key role in modern theoretical astrophysics, computing facilities let us evolve systems of equations to uncover how a system would evolve with certain conditions. In this thesis I present my project done at the Hamburg Observatory, where I performed hydrodynamical simulations trying to reproduce a newly discovered bizarre object called Pa 30. The first observations of Pa 30 were back in August of 1181, when Chinese and Japanese observed a guest star, a manifestation of a cataclysmic variable star, today we refer to the event as SN1181. The event was a Supernova Iax a rare and poorly known SN event, 843 years later [SII] λλ6716, 6731 observations performed on the supernova remnant unveiled a unique morphology, different from other well known supernova remnants. The structure of Pa 30 Supernova remnant is not chaotic as usual SNR, it presents a set of radially aligned filaments of gas, the formation mechanism of this structure is currently unknown. In this project I learned to use Athena++, a state-of-the-art fluid dynamics code designed for astrophysics, to investigate what we thought was the simplest explanation for the filaments formation: cold gas stripped from outflowing wind. The work consisted in creating a problem generator that was suited for the problem, perform simulations and analyze them. This thesis is structured in chapters, starting with a general overview to the astrophysical object of interest, then an introduction to the basic fluid dynamics topics related to the problem, a presentation on how Athena works and what I implemented on it, the results of the simulations and a conclusion.