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Lee Hartmann, University of Michigan
Andi Burkert, John Tobin, Marina Kounkel, Fred Adams
ONC: kinematics etc.
large-scale AV map
Rowles & Froebrich 2009
Orion A/B
3
Non-linear acceleration vs. position in filaments
(Bonnell et al 1992)- “edge effect” in ~ 1 dimension
make concentrations (clusters) at ends
acce
lera
tion
Evidence for large-scale gravity; focusing in elongated clouds causes clusters to form preferentially at ends
(Bonnell; Burkert & LH, “focal points”)
Pipe (Lombardi)
NGC 2264 (Sung+)
Perseus (Rebull)
Orion A/B
13CO, Bally et al.
Orion A (Hartmann & Burkert 2007); elliptical sheet, smooth density gradient, ~ 2 Myr evolution
cluster
Short radius of curvature results in extra mass
concentrations assemble cluster
gas/stars
Carpenter + 2001
1 pc
1 pc HH98,
e ~ 0.3
RV
1pc/2 km/s ~ 0.5 Myr
(2GM/R)1/2 ~ 3 km/s (4000 M☉/4 pc)1/2
fixed gas potential; N body
spherical, subvirial elongated, subvirial, major axis
elongated, subvirial, 30o
elongated, virial, 30o
Megeath et al.
caustic? why only one side?
asymmetry of mass distribution?
histogram = *
13CO
Jones & Walker 88 1D FWHM (proper motion)
ONC
Foreground contamination?
Briceno et al.
What accounts for the stellar/13CO velocity offset?
stellar motions? stars moving away from us too extincted for optical study?
<
problem? velocity widths already seem to be ≥ Jones/Walker p.m. dispersion
What accounts for the stellar/13CO velocity offset?
evaporation/blowout of dense gas?
<
works for ONC/1977(?), but what about OMC 2/3?
What accounts for the stellar/13CO velocity offset?
gravitational collapse + dissipation
to make narrow filament?
<
OMC 2/3?
crazy idea; “some stars left behind?”
1st generation less redshifted (running into denser gas)?
later generation?
need to understand time evolution of region
NGC 2264 – Kounkel, Tobin et al. in prep
?
kinematics:
not equilibrium – constraint on timescales?
gravity is important, but details uncertain
need to understand time evolution of region
histogram = *
13CO
foreground 1a pop?
27 Orion A 13CO; Bally et al. 1987
Velocity fields not particularly random
30 pc
(G x 105 M(sun)/15 pc)1/2 ~ 5 km/s
how do you avoid gravitationally-generated motion??
factor in efficiency; pre-existing cloud structure?
ages of ONC stars??
Heitsch
Vazquez-S.
Simulations of cloud flow with gravity show accelerating collapse
Orion Nebula regionMegeath et al. 2012
T Tauri stars
Protostars: collapse down
to extremely dense filament Pgrav >> P(ISM)