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Zooming in on the Formation of Protoplanetary Disks

Published online by Cambridge University Press:  06 January 2014

Åke Nordlund ,
Troels Haugbølle ,
Michael Küffmeier ,
Paolo Padoan  and
Aris Vasileiades
Åke Nordlund
Affiliation:
Centre for Star and Planet Formation, University of Copenhagen, Øster Voldgade 5, DK-2100 Copenhagen, Denmark email: aake@nbi.dk Niels Bohr Institute, University of Copenhagen Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark
Troels Haugbølle
Affiliation:
Centre for Star and Planet Formation, University of Copenhagen, Øster Voldgade 5, DK-2100 Copenhagen, Denmark email: aake@nbi.dk
Michael Küffmeier
Affiliation:
Centre for Star and Planet Formation, University of Copenhagen, Øster Voldgade 5, DK-2100 Copenhagen, Denmark email: aake@nbi.dk Niels Bohr Institute, University of Copenhagen Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark
Paolo Padoan
Affiliation:
ICREA & ICC, University of Barcelona, Marti i Franqus 1, E-08028 Barcelona, Spain
Aris Vasileiades
Affiliation:
Centre for Star and Planet Formation, University of Copenhagen, Øster Voldgade 5, DK-2100 Copenhagen, Denmark email: aake@nbi.dk Niels Bohr Institute, University of Copenhagen Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark
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Abstract

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We use the adaptive mesh refinement code RAMSES to model the formation of protoplanetary disks in realistic star formation environments. The resolution scales over up to 29 powers of two (~ 9 orders of magnitude) covering a range from outer scales of 40 pc to inner scales of 0.015 AU. The accretion rate from a 1.5 solar mass envelope peaks near 10−4 M⊙ about 6 kyr after sink particle formation and then decays approximately exponentially, reaching 10−6 M⊙ in 100 kyr. The models suggest universal scalings of physical properties with radius during the main accretion phase, with kinetic and / or magnetic energy in approximate balance with gravitational energy. Efficient accretion is made possible by the braking action of the magnetic field, which nevertheless allows a near-Keplerian disk to grow to a 100 AU size. The magnetic field strength ranges from more than 10 G at 0.1 AU to less than 1 mG at 100 AU, and drives a time dependent bipolar outflow, with a collimated jet and a broader disk wind.

Keywords

ISM: magnetic fieldsjets and outflowsstars: formationplanetary systems: formationaccretion disks
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. 131 - 135
Copyright
Copyright © International Astronomical Union 2013 

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