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Conference Paper

Resolving the Magnetic Field of IRAS 16293-2422 with ALMA

MPS-Authors

Sadavoy,  Sarah
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Myers,  Philip
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Stephens,  Ian W.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Tobin,  John
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Kwon,  Woojin
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Segura-Cox,  Dominique
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Henning,  Thomas K.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Commercon,  Benoit
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Looney,  Leslie
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

External Resource

https://ui.adsabs.harvard.edu/abs/2019AAS...23312702S
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Citation

Sadavoy, S., Myers, P., Stephens, I. W., Tobin, J., Kwon, W., Segura-Cox, D., et al. (2019). Resolving the Magnetic Field of IRAS 16293-2422 with ALMA. In American Astronomical Society Meeting Abstracts #233.


Cite as: https://hdl.handle.net/21.11116/0000-0005-D26E-3
Abstract
We present ALMA high-resolution dust polarization observations of IRAS 16293-2422. The dust polarization and inferred magnetic field are well resolved across the protostellar sources and the filamentary structures seen between them. The magnetic field is aligned parallel to the filamentary structures rather than showing a pinched morphology expected for accreting stars. We construct a simple toy model to investigate the energy balance in the filamentary bridge of dust and gas between the stars. We find high gas flow rates such that the bridge should be short- lived, and we propose that it is either a transient structure or must otherwise accrete new material. The parallel magnetic fields seen in IRAS 16293 are an unique feature and future theoretical work will need to understand both their origin and their impact on the evolution of young stars.