Magnetic fields from filaments to cores

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:	Physics and Astronomy
Subjects:	Q Science > QB Astronomy
Publisher:	Fabrizio Serra editore
ISSN:	0037-8720
Related URLs:	Organisation
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