protostellar disks: birth, life and death
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National Aeronautics and Space Administration. Protostellar Disks: Birth, Life and Death. Neal Turner Jet Propulsion Laboratory, California Institute of Technology. The Life of Protostellar Disks. Jets and Winds Basic disk properties - PowerPoint PPT PresentationTRANSCRIPT
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Neal Turner Jet Propulsion Laboratory, California Institute of Technology
Protostellar Disks: Protostellar Disks: Birth, Life and DeathBirth, Life and Death
National Aeronautics and Space Administration
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The Life of Protostellar Disks
1. Jets and Winds2. Basic disk properties3. Angular momentum transport4. Evolution of the solids
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National Aeronautics and Space Administration
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Hartigan et a
l. 1995 / A
ntoniucci et al. 2008
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McKee & Ostriker 2007
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Pyo et al. 2005
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Zinnecker et al. 1998
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Takam
i et al. 2001
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Burrow
s et al. 199
6
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C. Lad
a 1985
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Girart et al. 2006
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Tam
ura et al. 1999
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T. R
ay et al. 1997
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Johns-Krull 2007
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Ferreira et al. 2006
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Spruit 1996National Aeronautics and Space Administration
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Anderson et al. 2003
Size of the Launching Region?
Jet power = Rate of work done against the magnetic torque= (Footpoint orbital frequency) x (Angular momentum flux):
€
v p,∞2
2= Ω0ϖ∞vφ ,∞
Infer launching region lies 0.3 to 4 AU from the star.
Assumes energy and momentum conserved along streamlines.
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Y. Kato 2004
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Nakam
ura &
Li 20
07
Outflow-Driven Turbulence 1
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Outflow-Driven Turbulence 2
Cloud kinetic energy vT2 dissipates on a crossing time R/vT, so
the outflows can provide the stirring if
With R=10 pc, vT=10 km s-1, f=0.01, vJ=300 km s-1 and jet mass flow rate 10-7 Solar masses per year,
the outflows are sufficient to power the turbulence.
i.e., if the outflow kinetic luminosity is greater than the dissipation rate in the gas associated with the star.
€
M•
J vJ2 >
M*vT2
f
vT
R
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Basic Disk Properties
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Hartmann & Kenyon 1996National Aeronautics and Space Administration
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M. Simon et al. 2000
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Andrews & Williams 2007National Aeronautics and Space Administration
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Andrews & Williams 2007National Aeronautics and Space Administration
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Origins of the Surface Density Profile
In steady-state Shakura-Sunyaev -disk,
€
Σ ~M
•
ν~
M•
Ωμ
αT~ R−1
if irradiation controls the temperature profile.
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Weidenschillin
g 1977
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Dullemond et al. 2007National Aeronautics and Space Administration
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Dullemond et al. 2007National Aeronautics and Space Administration
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Dullemond et al. 2007National Aeronautics and Space Administration
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Bergin et al. 2007National Aeronautics and Space Administration
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K. R. Bell et al. 1995National Aeronautics and Space Administration
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Hartmann et al. 1993National Aeronautics and Space Administration
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Angular Momentum Transport
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1. Gravitational Instability1. Gravitational Instability
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1. Gravitational Instability1. Gravitational Instability
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Small disturbances grow if
r
H
M
r
Σ
*
2
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Gam
mie 2001
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Gam
mie 2001
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Mejia et al. 2005
With slower cooling, instability leads to sustained accretion.
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Balbus &
Haw
ley 1991
2. M
agn
eto
-Ro
tati
on
al
2. M
agn
eto
-Ro
tati
on
al
Tu
rbu
len
c eT
urb
ule
nce
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Az
c
v 2B
albus & H
awley 1991
2. M
agn
eto
-Ro
tati
on
al
2. M
agn
eto
-Ro
tati
on
al
Tu
rbu
len
c eT
urb
ule
nce
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Ga
mm
ie 1
99
6
Na
tion
al A
ero
na
utic
s a
nd
Sp
ace
Ad
min
istr
atio
n
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Three Ways to Lose Magnetic Flux
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Ionization ProcessesIonization Processes
Stellar X-Rays
Interstellar Cosmic Rays
Long-Lived Radionuclides
At 1 AU in the minimum mass
Solar nebula
Midplane ionisation is weak!
Short-Lived Radionuclides
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Wardle 2007National Aeronautics and Space Administration
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1
2Azv
Sa
no
& S
ton
e 2
00
2b
MRI turbulence requires
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1 m Grains
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No Grains
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H. Li et al. 2001
P
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Lodato & Clarke 2004National Aeronautics and Space Administration
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Evolution of the Solids
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van Boekel et al. 20
04
Na
tion
al A
ero
na
utic
s a
nd
Sp
ace
Ad
min
istr
atio
n
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van Boekel et al. 20
04
Na
tion
al A
ero
na
utic
s a
nd
Sp
ace
Ad
min
istr
atio
n
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TEM image of a thin-sectioned Wild 2 grain consisting of enstatite with exsolution lamellae of diopside, formed from a melt (H. Leroux)
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Natta et al. 20
07
ResolvedUnresolved
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Furlan et al. 200
6
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Da
hm
& H
illen
bra
nd
20
07
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Du
llem
on
d &
Do
min
ik 20
04
Set
tlin
g is
rap
id in
a la
min
ar d
isk
Set
tlin
g is
rap
id in
a la
min
ar d
isk
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A Rough Estimate of Grain Growth Timescales
Particles settle at the terminal speed, with the force of gravity balancing the force of the gas molecules striking from below:
Particles remain compact spheres.
Particles grow by sweeping up smaller, stationary grains:
€
dz
dt= vsett =
−mg
ρcsσ
€
dm
dt=10−2 ρvsettσ
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Settling Only
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Settling & Sweeping
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Particle growth: extreme cases
BPCA
Ballistic Particle-Cluster Agglomeration
⇓
ballistic hit-and-stick impacts of single dust particles into growing
dust agglomerate
BCCA
Ballistic Cluster-Cluster Agglomeration
⇓
ballistic hit-and-stick collisions between equal-mass dust
agglomerates
i = 1,024 i = 1,024From J. Blum
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BPCAN=2
From J. Blum
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BPCAN=4
From J. Blum
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BPCAN=8
From J. Blum
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BPCAN=16
From J. Blum
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BPCAN=32
From J. Blum
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BPCAN=64
From J. Blum
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BPCAN=128
From J. Blum
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BPCAN=256
From J. Blum
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BPCAN=512
From J. Blum
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BPCAN=1024
From J. Blum
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BCCAN=2
From J. Blum
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BCCAN=4
From J. Blum
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BCCAN=8
From J. Blum
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BCCAN=16
From J. Blum
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BCCAN=32
From J. Blum
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BCCAN=64
From J. Blum
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BCCAN=128
From J. Blum
National Aeronautics and Space Administration
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From J. Blum
National Aeronautics and Space Administration
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From J. Blum
National Aeronautics and Space Administration
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From J. Blum
National Aeronautics and Space Administration
![Page 85: Protostellar Disks: Birth, Life and Death](https://reader036.vdocument.in/reader036/viewer/2022062518/56814a93550346895db7a0a5/html5/thumbnails/85.jpg)
Radial Drift
Hot, Dense
Cold, Less
Dense
National Aeronautics and Space Administration
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Radial Drift
Hot, Dense
Cold, Less
Dense€
vφ2 = vK
2 +R
ρ
∂P
∂R
≈ vK2 − cs
2
vφ ≈ 1−H 2
2R2
⎛
⎝ ⎜
⎞
⎠ ⎟vK
National Aeronautics and Space Administration
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Radial Drift
Hot, Dense
Cold, Less
Dense
Grain v=vK
National Aeronautics and Space Administration
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Weidenschilling &
Cuzzi 1993
1 AU in MMSN
National Aeronautics and Space Administration
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Non-fractal Aggregate Growth
(Hit-and-Stick)
Cratering/Fragmentatio
n
Non-fractal Aggregate Sticking + Compaction
Cratering/Fragmen-tation/Accretion
Non
-fra
cta
l A
gg
reg
ate
S
tickin
g +
Com
pacti
on
Frac
tal A
ggre
gate
Growth
(Hit-
and-
Stick)
Restructuring/Compaction
Frag
men
tatio
n
»0
«0
EXPERI
MENTS
Bounc
ing
Non
-fra
cta
l A
gg
reg
ate
G
row
th(H
it-a
nd
-Sti
ck)
Cra
teri
ng
/Fra
gm
en
-ta
tion
/Accre
tion
Cra
teri
ng
/Fra
gm
en
tati
on
Erosion
Ero
sio
n
A
COMPILATION
Fro
m J
. B
lum
National Aeronautics and Space Administration
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Diameter
Dia
mete
r
1 µm
100 m
100 µm
1 cm
1 m
1 µm 100 m100 µm 1 cm 1 m
Non-fractal Aggregate Growth
(Hit-and-Stick)
Erosion
Non
-fra
cta
l A
gg
reg
ate
S
tickin
g +
Com
pacti
on
Cra
teri
ng
/Fra
gm
en
-ta
tion
/Accre
tion
Cratering/Fragmentatio
n
Frac
tal A
ggre
gate
Growth
(Hit-
and-
Stick)
Restructuring/Compaction
Bounc
ing
Frag
men
tatio
n
»0
«0
Ero
sio
nN
on
-fra
cta
l A
gg
reg
ate
G
row
th(H
it-a
nd
-Sti
ck)
Non-fractal Aggregate Sticking + Compaction
Cratering/Fragmen-tation/Accretion
Cra
teri
ng
/Fra
gm
en
tati
on Mass
loss
Mass conservation
Mass gain
**
**
* for compact
targets only
Blum & Wurm 2008
National Aeronautics and Space Administration
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Barranco 2008
Stirring by Kelvin-Helmholtz Instability
National Aeronautics and Space Administration
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Stirring by Magneto-Rotational Turbulence
Turner et al. 2006
National Aeronautics and Space Administration
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Sti
rrin
g b
y 2-
Str
eam
Inst
abili
ty
Johansen et al. 2007
National Aeronautics and Space Administration
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The Life of Protostellar Disks
1. Jets and Winds2. Basic disk properties3. Angular momentum transport4. Evolution of the solids
National Aeronautics and Space Administration