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Magnetic fields from filaments to cores

Koch, P. M., Tang, Y.-W., Chapman, N.L., Duarte Cabral Peretto, Ana ORCID:, Ho, P.T.P., Novak, G., Peretto, Nicolas ORCID:, 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.

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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:
Date of First Compliant Deposit: 10 May 2018
Date of Acceptance: 22 January 2018
Last Modified: 23 Oct 2022 13:40

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