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MIAPP - Presentation

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Michael Küffmeier

on 7 September 2017

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Transcript of MIAPP - Presentation

Zooming in on protoplanetary disk formation
astrobites.org
Michael Küffmeier
Heterogeneous accretion
Accretion ...
...
differs from star to star
... is
heterogeneous in time
(episodic events due to infall and disk)
... is
heterogeneous in space
around each individual star
Hammer projection
r=50 AU, t=100 kyr after star formation

Outflow
Infall
In Practice
Start from
snapshot of young Giant Molecular Cloud obtained by
previous simulation
(40 pc) box (AMR, ideal MHD)

Mimic stars with
sink particles

Zoom experiments with different refinement level
Credit: Åke Nordlund
My main points
Suggestion:
Protostellar environments influence the shape of planetary systems
My main points
Zoom-simulations are necessary
to account for difference in protostellar environments
Suggestion:
Diversity of protostellar environments causes variety of planetary systems
Procedure
Parental run with
level 16 (min cell size 126 AU)
3
Possible consequence for planet formation
Short disk lifetimes (e.g.
Mamajek 2009
) suggest early planet formation
Enhanced mass

reservoir
to form planets?
+
Protostellar
accretion
is a
heterogeneous
process in space and in time
Protostellar
accretion
is a
heterogeneous
process in space and in time
0
4 Myr
t - ~10 kyr
100 kyr
Zoom-in to
level 22 (2 AU)
t
0
Disk size and disk mass
radius where azimuthal velocity drops below 85 % of the Kepler speed
mass enclosed within disk radius and height +/- 8 AU
0
40 pc
40 pc
~4 kAU
~100 AU
l
o
g
l
i
n
e
a
r
References:
Kuffmeier et al. 2016, ApJ
Kuffmeier, Haugbølle & Nordlund submitted
Possibility of large-scale infall
Carried out in
modified
version of RAMSES
Teyssier 2002
Fromang et al. 2006
Haugbølle and Nordlund
Zoom-simulations are necessary
to account for different protostellar environments
Everything solved?
Of course...
NOT!
Issues and challenges:
Sink
particles
Expensive!
(Resolution)
...
numerical
physical
Only
ideal MHD
No
radiative transfer
No
dust
No
chemistry
...
But important to constrain initial conditions of disk models!
Adaptive Mesh Refinement
MagnetoHydroDynamics
Turbulence
driven by supernovae
within sphere of 100 AU
Stellar environments at sink formation
Disk Surface density
t=50 kyr
Small scale episodicity due to disk instabilities
Kuffmeier, Jensen, Frimann and Haugbølle in prep
Account for formation history of disks in modeling planet formation
with code framework DISPATCH
Nordlund, Ramsey, Popovas and Kuffmeier 2017
Troels Haugbølle, Åke Nordlund
Disk Formation and evolution
Sketches:

M. Persson
Star Formation community
Disk and planet community
What's the effect of the environment on the disk properties?
Credit: Paolo Padoan
Stars form in different environments
See also:
Stamatellos+ 2011,2012
Dunham & Vorobyov 2012
Liu+ 2016
Accretion is heterogeneous
like brewing filter coffee
Infall
Disk
Star
Different environment = different disk
50 kyr after star formation
Origin of tracer particles
Disk
formation
determined by
turbulence and magnetic braking
Seifried et al. 2013, Li et al. 2014
Please find the complete presentation including movies under the link below:
http://prezi.com/5uvlyzmj6txa/?utm_campaign=share&utm_medium=copy&rc=ex0share
Full transcript