Winds that Sail on Starlight Stan Owocki Bartol Research Institute University of Delaware...
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Transcript of Winds that Sail on Starlight Stan Owocki Bartol Research Institute University of Delaware...
Winds that Sail on Starlight
Stan Owocki
Bartol Research Institute
University of DelawareCollaborators:
– Asif Ud-Doula, U. Delaware
– Vikram Dwarkadas, U. Del.
– Ken Gayley, U. Iowa
– David Cohen, Swarthmore
– Steve Cranmer, CfA
– Joachim Puls, U. Munich
– Luc Dessart, Utrecht
– Mark Runacres, U. Brussels
2Winds that Sail on StarlightSTScI 11/07/01
Wind-Blown Bubbles in ISM
Some key scalings:
WR wind bubble NGC 2359 Superbubble in the
Large Magellanic Cloud
Henize 70: LMC SuperBubble
3Winds that Sail on StarlightSTScI 11/07/01
Pistol Nebula
4Winds that Sail on StarlightSTScI 11/07/01
Eta Carinae
STScI 11/07/01 Winds that Sail on Starlight 5
P-Cygni Line Profiles
STScI 11/07/01 Winds that Sail on Starlight 6
Sailing vs. Radiative Driving
• Modern sails– asymmetric form + keel
– can tack against wind
– unstable to “keeling over”
• Line-driving ca. 2000– asymmetric velocity
gradient
– force not || flux• spindown & disk inhibition
• ablation & disk winds
– radiative braking
– small-scale instability
• CAK 1975– 1D spherically symmetric
– radially driven outflow
• Early sails – symmetric form
– sail mainly with wind
STScI 11/07/01 Winds that Sail on Starlight 7
• Light transports energy (& information)
• But it also has momentum, p=E/c
• Usually neglected, because c is so high
• But becomes significant for very bright objects,
e.g. Lasers, Hot stars,
QSO/AGN’s
• Key question: how big is force vs. gravity??
Light’s Momentum
STScI 11/07/01 Winds that Sail on Starlight 8
Free Electron Scattering
Thompson Cross Section
th
e-
Th= 2/3 barn= 0.66 x 10-24 cm2
STScI 11/07/01 Winds that Sail on Starlight 9
• How big is electron scattering force vs. gravity??
• Expressed through a star’s Eddington parameter
~
gel
ggrav
eL4GMc
Eddington Parameter
• For sun, O ~ 2 x 10-5
• But for hot-stars with L~ 106 LO ; M=10-50 MO
r
L4 r2c
Th
e
GM2
STScI 11/07/01 Winds that Sail on Starlight 10
Q~ ~ 1015 Hz * 10-8 s ~ 107
Q ~ Z Q ~ 10-4 107 ~ 103
Line Scattering: Bound Electron Resonance
lines~Q Th
glines~103g el
LLthin} iflines
~103
el 1
for high Quality Line Resonance,
cross section >> electron scattering
STScI 11/07/01 Winds that Sail on Starlight 11
Optically Thick Line-Absorption in an Accelerating Stellar Wind
gthick~gthin
τ~
1ρ
dvdr
τ≡κρvth
dv/dr
LsobFor strong,
optically thick lines:
STScI 11/07/01 Winds that Sail on Starlight 12
CAK model of steady-state wind
inertia gravity CAK line-accel.
Equation of motion: v ′ v ≈−GMr2 +
fQ Lr2
r2v ′ v ˙ M Q
⎛
⎝ ⎜ ⎜
⎞
⎠ ⎟ ⎟ α < 1
CAK ensemble ofthick & thin lines
˙ M ≈Lc2
Q−⎛
⎝⎜
⎞
⎠⎟
−Mass loss rate
˙ M v∞ ∝ L1
αWind-Momentum
Luminosity Law
≈0.6
v(r) ≈v∞(1−R∗/r)Velocity law
~vesc
* fix M to make line-accel. order gravity *.
STScI 11/07/01 Winds that Sail on Starlight 15
Wolf-Rayet Winds• “Momentum #” =Mv/(L/c) > 1
• Requires multiple scattering
.
Need line spacing overlap v/v= > 1
STScI 11/07/01 Winds that Sail on Starlight 17
Inward-propagating Abbott waves
±v ª ei(k r ° ! t)
°@v0
i!±v =@grad ±v0
¥ U ik±v
w=k= ° U
U =@grad
@v0
ªgrad
v0 ªvv0
v0 ª v
ad@v@t
= gr
v
r
g~ v’
Abbott speed
STScI 11/07/01 Winds that Sail on Starlight 18
Pulsation-induced wind variability
Velocity
Radius
radiative drivingmodulated by
brightness variations
Abbott-mode“kinks”
velocity “plateaus”
shockcompression
STScI 11/07/01 Winds that Sail on Starlight 20
BW Vul: Observations vs. Model
C IV Model line
STScI 11/07/01 Winds that Sail on Starlight 21
HD64760 Monitored duringIUE “Mega” Campaign
Monitoring campaigns of P-Cygni lines formed in hot-star winds also often show modulation at periods comparable to the stellar rotation period.
These may stem from large-scale surface structure that induces spiral wind variation analogous to solar Corotating Interaction Regions.
Radiation hydrodynamicssimulation of CIRs in a hot-star wind
Rotational Modulation of Hot-Star Winds
STScI 11/07/01 Winds that Sail on Starlight 23
Line-Driven Instability
u=v/vth
for < Lsob:
g ~ u
Instability with growth rate
~ g/vth ~ v/Lsob ~100 v/R
=> e100 growth!
STScI 11/07/01 Winds that Sail on Starlight 26
Time snapshot of wind instability simulation
0.0 0.5 1.0
0
500
1000
1500
-15
-14
-13
-12
-11
-10
Height (R*
)
Velocity
Density
CAK
STScI 11/07/01 Winds that Sail on Starlight 30
modelDessart
& Owocki
2002
WR Star Emission Profile Variability
WR 140Lepine &
Moffat 1999
STScI 11/07/01 Winds that Sail on Starlight 32
WR+O Colliding wind
*WR Star
O Star
“Radiative Braking”
Pure Hydro
*WR Star
O Star
RadiationHydro
e.g., V444 Cygni
36Winds that Sail on StarlightSTScI 11/07/01
Gravity Darkeningincreasing stellar rotation
fast dense wind
slower windslower wind
STScI 11/07/01 Winds that Sail on Starlight 37
Formation of Prolate Nebulae
-limit
Langer et al. 1999:Fast spherical wind into slow, dense equatorial flow
Dwarkadas et al. 2001Prolate fast wind into spherical medium
Gravity darkening
STScI 11/07/01 Winds that Sail on Starlight 40
Wind Compressed Disk SimulationsVrot (km/s) = 200 250 300 350 400 450
radial forcesonly
WCD Inhibition by non-radial
line-forces
STScI 11/07/01 Winds that Sail on Starlight 41
Vector Line-Force
r g line ~ d
*
∫rn I*
rn⋅[∇(
rn⋅
rv)]
dvn/dn
Net poleward line force from:
fasterpolarwind
slower equatorial wind
r
Max
[dv n
/dn]
(2) Pole-equator aymmetry in velocity gradient
r
Flux
(1) Stellar oblateness => poleward tilt in radiative flux
N
STScI 11/07/01 Winds that Sail on Starlight 42
Wind rotation spindown from
azimuthal line-torque
g
(10 3 cm/s 2 )
[V
(nrf) - V
(wcd)]
*sin( )*r/Req
(km/s)
a. b.
-10
-30
-50
-70
-90
-0.1
-0.3
-0.5
-0.7
-0.9
azimuthalline-force
ang. mom.loss
STScI 11/07/01 Winds that Sail on Starlight 43
I + I -I +
I +
I -
I -
Azimuthal Line-Torque
V+ <V_
g~V+ -V_ <
STScI 11/07/01 Winds that Sail on Starlight 44
Line-Force in Keplerian Disk
r
dvr/dr z
dvz/dz
STScI 11/07/01 Winds that Sail on Starlight 45
Accretion Disk Windsfrom BAL QSOs
blackhole
Xraysource
UV
failed windX-ray shield
UV line-drivenAccretion Disk Wind
radiatingaccretion
disk
STScI 11/07/01 Winds that Sail on Starlight 46
Line-Driven Ablation
g lines ~ dv l
/dl
Net radiative Flux = 0, but glines ~ dvl/dl > 0 !
STScI 11/07/01 Winds that Sail on Starlight 47
Be disk formation by RDOME(Radiatively Driven Orbital Mass Ejection)
STScI 11/07/01 Winds that Sail on Starlight 49
MHD simulation of line-driven windZoom on densityDensityY- Velocity
-1000 vy (km/s) 1000
STScI 11/07/01 Winds that Sail on Starlight 51
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295 G ; * = 1
Final state of ZPup isothermal models
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1650 G ; * = 32 930 G ; * = 10
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520 G ; * = 3.2
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165 G ; * = 0.32
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93 G ; * = 0.1
STScI 11/07/01 Winds that Sail on Starlight 52
Summary• Lines efficient way for radiation to drive mass
– force depends of l.o.s. velocity gradient
– for non-spherical geometry, anisotropic opacity
– can get spindown, ablation, WCD inhibition, radiative braking, disk winds
• Line-driving very unstable for < LSob << R*
– leads to shocks, clumping, compressible turbulence
– may explain X-rays
• Current work– effect of NRP, B-field on wind
– application to BAL QSO/AGN disk winds
– formation of Be disks
– Super-Eddington Luminous Blue Variables