Towards a complete understanding of the Magellanic Stream Formation
Date Issued
2019
Author(s)
Wang, Jianling
•
Hammer, Francois
•
Yang, Yanbin
•
•
Cioni, Maria-Rosa L.
•
Puech, Mathieu
•
Flores, Hector
Abstract
The Magellanic Clouds (MCs) have lost most of their gas during their passage by the Milky Way, a property that has never been successfully modelled. Here, we use accurate and mesh-free hydrodynamic simulations to reproduce the Magellanic Stream and the MCs in the frame of a `ram-pressure plus collision' model. This model reproduces many of the observed properties of the H I 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 H I gas consistent with those observed. The modelled 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.
Volume
486
Issue
4
Start page
5907
Issn Identifier
0035-8711
Ads BibCode
2019MNRAS.486.5907W
Rights
open.access
File(s)![Thumbnail Image]()
Loading...
Name
wang2019.pdf
Description
PDF editoriale
Size
6.05 MB
Format
Adobe PDF
Checksum (MD5)
6898b481dd4dc772e67df51aa1fde4b6