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The Early Era: How do protostellar discs form?

Published online by Cambridge University Press:  06 January 2014

Marc Joos ,
Patrick Hennebelle ,
Andrea Ciardi  and
Sébastien Fromang
Marc Joos
Affiliation:
Service d'Astrophysique (CEA/DSM/Irfu/SAp) Laboratoire de Radioastronomie, ENS - LERMA, Observatoire de Paris, Universit Pierre et Marie Curie
Patrick Hennebelle
Affiliation:
Service d'Astrophysique (CEA/DSM/Irfu/SAp) Laboratoire de Radioastronomie, ENS - LERMA, Observatoire de Paris, Universit Pierre et Marie Curie
Andrea Ciardi
Affiliation:
Laboratoire de Radioastronomie, ENS - LERMA, Observatoire de Paris, Universit Pierre et Marie Curie
Sébastien Fromang
Affiliation:
Service d'Astrophysique (CEA/DSM/Irfu/SAp)
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Abstract

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Discs are a key element in star and planet formation; however, magnetic fields can efficiently transport angular momentum away from the central region of the collapsing core during the dense core collapse, preventing disc formation. We perform numerical simulations of magnetically supercritical collapsing cores with a misalignment between the rotation axis and the magnetic field (Joos et al. 2012) and in a turbulent environment (Joos et al. 2013). The early formation of massive discs can take place at moderate magnetic intensities if the rotation axis is tilted or in a turbulent environment, because of misalignment and turbulent diffusion.

Keywords

star formationlow mass starsdisc formationmagnetohydrodynamicsturbulencenumerical simulations
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S299: Exploring the Formation and Evolution of Planetary Systems , June 2013 , pp. 163 - 164
Copyright
Copyright © International Astronomical Union 2013 

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