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Zooming in on the Formation of Protoplanetary Disks

  • Åke Nordlund (a1) (a2), Troels Haugbølle (a1), Michael Küffmeier (a1) (a2), Paolo Padoan (a3) and Aris Vasileiades (a1) (a2)...
Abstract
Abstract

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.

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This list contains references from the content that can be linked to their source. For a full set of references and notes please see the PDF or HTML where available.

R. M. Crutcher 2011, ARAA, 50, 29

P. Goldreich & W. R. Ward 1973, ApJ, 183, 1051

R. Larson 1981, MNRAS, 194, 809

P. M. Solomon , A. R. Rivolo , J. Barrett , & A. Yahil 1987, ApJ, 319, 730

R. Teyssier 2002, A&A, 385, 337

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Proceedings of the International Astronomical Union
  • ISSN: 1743-9213
  • EISSN: 1743-9221
  • URL: /core/journals/proceedings-of-the-international-astronomical-union
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