| dc.creator |
Duarte-Cabral, A |
|
| dc.creator |
Dobbs, CL |
|
| dc.date |
2018-11-23T15:36:31Z |
|
| dc.date |
2017-06-20 |
|
| dc.date |
2018-11-23T15:36:31Z |
|
| dc.date.accessioned |
2022-05-27T01:03:10Z |
|
| dc.date.available |
2022-05-27T01:03:10Z |
|
| dc.identifier |
Vol. 470, pp. 4261 - 4273 |
|
| dc.identifier |
10.1093/mnras/stx1524 |
|
| dc.identifier |
http://hdl.handle.net/10871/34892 |
|
| dc.identifier |
0035-8711 |
|
| dc.identifier |
Monthly Notices of the Royal Astronomical Society |
|
| dc.identifier.uri |
http://localhost:8080/xmlui/handle/CUHPOERS/241931 |
|
| dc.description |
This is the final version. Available from OUP via the DOI in this record |
|
| dc.description |
In recent years, there has been a growing interest in studying giant molecular filaments (GMFs), which are extremely elongated (> 100 pc in length) giant molecular clouds (GMCs). They are often seen as inter-arm features in external spiral galaxies, but have been tentatively associated with spiral arms when viewed in the Milky Way. In this paper, we study the time evolution of GMFs in a high-resolution section of a spiral galaxy simulation, and their link with spiral arm GMCs and star formation, over a period of 11 Myr. The GMFs generally survive the interarm passage, although they are subject to a number of processes (e.g. star formation, stellar feedback and differential rotation) that can break the giant filamentary structure into smaller sections. The GMFs are not gravitationally bound clouds as a whole, but are, to some extent, confined by external pressure. Once they reach the spiral arms, the GMFs tend to evolve into more substructured spiral arm GMCs, suggesting that GMFs may be precursors to arm GMCs. Here, they become incorporated into the more complex and almost continuum molecular medium that makes up the gaseous spiral arm. Instead of retaining a clear filamentary shape, their shapes are distorted both by their climbing up the spiral potential and their interaction with the gas within the spiral arm. The GMFs do tend to become aligned with the spiral arms just before they enter them (when they reach the minimum of the spiral potential), which could account for the observations of GMFs in the Milky Way. |
|
| dc.description |
ADC and CLD acknowledge funding from the European Research Council for the FP7 ERC starting grant project LOCALSTAR. ADC also acknowledges the support of the UK STFC consolidated grant ST/N000706/1. This work used the DiRAC Complexity system, operated by the University of Leicester IT Services, which forms part of the STFC DiRAC HPC Facility (www.dirac.ac.uk). This equipment is funded by BIS National E-Infrastructure capital grant ST/K000373/1 and STFC DiRAC Operations grant ST/K0003259/1. DiRAC is part of the National E-Infrastructure. This work also used the University of Exeter Supercomputer, a DiRAC Facility jointly funded by STFC, the Large Facilities Capital Fund of BIS and the University of Exeter. |
|
| dc.language |
en |
|
| dc.publisher |
Oxford University Press (OUP) / Royal Astronomical Society |
|
| dc.rights |
© 2017 The Authors.
Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved |
|
| dc.subject |
methods: numerical |
|
| dc.subject |
ISM: clouds |
|
| dc.subject |
galaxies: ISM |
|
| dc.subject |
galaxies: spiral |
|
| dc.subject |
galaxies: star formation |
|
| dc.title |
The evolution of giant molecular filaments |
|
| dc.type |
Article |
|