# Toward a Complete Understanding of the Magellanic Stream Formation

## TL;DR

This study uses advanced hydrodynamic simulations to successfully model the formation of the Magellanic Stream and related features, resolving longstanding questions about their origins and properties.

## Contribution

It introduces a comprehensive 'ram-pressure plus collision' model that accurately reproduces the Magellanic Stream and associated structures, addressing previous modeling challenges.

## Key findings

- Reproduces the density profile and dual filament structure of the HI Stream.
- Matches observed ionized and HI gas amounts through instabilities.
- Successfully models the Magellanic Bridge and Cloud collision effects.

## Abstract

The Magellanic Clouds have lost most of their gas during their passage by the Milky Way, a property that has never been successfully modeled. Here we use accurate and mesh-free hydrodynamic simulations to reproduce the Magellanic Stream and the Magellanic Clouds in the frame of a 'ram-pressure plus collision' model. This model reproduces many of the observed properties of the HI Stream including most of its density profile along its length and its dual filamentary structure. Besides this, ram-pressure combined with Kelvin-Helmholtz instabilities extracts amounts of ionized and HI gas consistent with those observed. The modeled scenario also reproduces the Magellanic Bridge, including the offset between young and old stars, and the collision between the Clouds, which is responsible of the very elongated morphology of the Small Magellanic Cloud along the line of sight. This model has solved most of the mysteries linked to the formation of the Magellanic Stream. The Leading Arm is not reproduced in the current model because it requires an alternative origin.