Zooming in on the formation of protoplanetary disks
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Zooming in on the formation of protoplanetary disks. / Nordlund, Åke; Haugbølle, Troels; Küffmeier, Michael; Paodoan, Paolo; Vasileiades, Aris.
I: Proceedings of the International Astronomical Union, Bind 8, Nr. 299, 06.01.2014, s. 131-135.Publikation: Bidrag til tidsskrift › Tidsskriftartikel › Forskning › fagfællebedømt
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TY - JOUR
T1 - Zooming in on the formation of protoplanetary disks
AU - Nordlund, Åke
AU - Haugbølle, Troels
AU - Küffmeier, Michael
AU - Paodoan, Paolo
AU - Vasileiades, Aris
PY - 2014/1/6
Y1 - 2014/1/6
N2 - 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 ($\sim$ 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 $10^{-4}$ $\mspy$ about 6 kyr after sink particle formation and then decays approximately exponentially, reaching $10^{-6}$ $\mspy$ 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.
AB - 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 ($\sim$ 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 $10^{-4}$ $\mspy$ about 6 kyr after sink particle formation and then decays approximately exponentially, reaching $10^{-6}$ $\mspy$ 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.
KW - astro-ph.SR
U2 - 10.1017/S1743921313008107
DO - 10.1017/S1743921313008107
M3 - Journal article
VL - 8
SP - 131
EP - 135
JO - Proceedings of the International Astronomical Union
JF - Proceedings of the International Astronomical Union
SN - 1743-9213
IS - 299
ER -
ID: 50621606