Koch, P. M., Tang, Y.-W., Chapman, N.L., Duarte Cabral Peretto, Ana  ORCID: https://orcid.org/0000-0002-5259-4774, Ho, P.T.P., Novak, G., Peretto, Nicolas ORCID: https://orcid.org/0000-0002-6893-602X, Su, Y.-N., Takakuwa, S. and Yen, H.-W.
2018.
Magnetic fields from filaments to cores.
Presented at: Francesco's Legacy: Star Formation in Space and Time,
Florence, Italy,
5-9 June 2017.
Memorie della SAIt.
Journal of the Italian Astronomical Society / Memorie Della Società Astronomica Italiana.
, vol.88
Fabrizio Serra editore,
pp. 557-559.
|
Preview |
PDF
- Accepted Post-Print Version
Download (3MB) | Preview |
Abstract
How important is the magnetic (B-) field when compared to gravity and turbulence in the star-formation process? Does its importance depend on scale and location? We summarize submm dust polarization observations towards the large filamentary infrared dark cloud G34 and towards a dense core in the high-mass star-forming region W51. We detect B-field orientations that are either perpendicular or parallel to the G34 filament axis. These B-field orientations further correlate with local velocity gradients. Towards three cores in G34 we find a varying importance between B-field, gravity, and turbulence that seems to dictate varying types of fragmentation. At highest resolution towards the gravity-dominated collapsing core W51 e2 we resolve new B-field features, such as converging B-field lines and possibly magnetic channels.
| Item Type: | Conference or Workshop Item (Paper) |
|---|---|
| Status: | Published |
| Schools: | Schools > Physics and Astronomy |
| Subjects: | Q Science > QB Astronomy |
| Publisher: | Fabrizio Serra editore |
| ISSN: | 0037-8720 |
| Related URLs: | |
| Date of First Compliant Deposit: | 10 May 2018 |
| Date of Acceptance: | 22 January 2018 |
| Last Modified: | 23 Oct 2022 13:40 |
| URI: | https://orca.cardiff.ac.uk/id/eprint/111361 |
Actions (repository staff only)
 |
Edit Item |
Download Statistics
Download Statistics