outflows and jets - universität zu köln
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Star formation
Outflows and jets
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Observations of outflows and jets
• Optically detected jets:– Very collimated streams of gas, moving at supersonic speed
(~100 km/s)
– Mostly bipolar, mostly perpendicular to disk
Jet outflow rate typically 10-9... 10-7 M⊙.
• Molecular outflows:– Detected in CO lines
– Less colimated
– Often associated with optical jets (i.e. same origin)
Derived mass: 0.1...170 M⊙: large!• Most of accelerated mass must have been swept up from the cloud
core, rather than originating in mass ejected from the star
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Herbig-Haro objects
Most prominent outflow products● Radiation from excited hydrogen● Shock interaction of jet with surrounding cloud
HH 1 and 2
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Jet powered by the embedded source VLA1
x
VLA 1
HH1
HH2blue-shifted jet
green: Hα, red: SII
~ 0.1 pc
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Jets are observable in lines of ionized atoms
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HH 34 HH 47
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HH 30First direct observation of temporal changes
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HH 30Association with molecular gas in disk and outflow
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HH211: a well collimated low mass flow
● Many jets only de-tected in the In-frared
● Complementary CO observations “fill” the outflow pattern
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HH 212 Dragon
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The BHR71 Bok globule
Bourke et al. (1997)CO (1-0) outflow, powered by a class 0
protostellar binary (Lbol ~ 9 L⊙)
© J. Alves et al. (ESO Messenger 103)
I band
Tkin=11K
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Mapping of the outflow with APEXAPEX - Chajnantor
2MASS J band image
Parise et al. 2006CO(3-2)
IRAS 11590-6452: a binary protostellar system (ISO observations,Myers & Mardones 1998)
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CO(3-2) channel maps
imaging of the second outflow !
redshifted
blueshifted
APEX
precession ?
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Velocity structure traced by COT ~ 30-40 K
T ~ 50 K
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Physical diagnostic using methanol
30 <T< 50 K105 <n< 3.105
T ~ 20-30 Kn ~ 105 cm-3
T ~ 10K
preshock gas ?
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IRAS 19410: how high resolution changes the picture
from 2 to 6 cores; from 2 to 9 flows
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Molecular Outflows
Numerous out-flows show a rela-tively wide angle
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Jets and Outflows
● Most dramatic phenomenon as evidence of star formation.
● Common phenomenon from proto-brown dwarfs (with 0.03 M⊙) up to very massive stars (10 M⊙)
● For low mass stars, flows of younger stars are
● faster
● more highly collimated
● Influence the surrounding material both mechanically and thermally.
● Contrary to the disks, jets and outflows were not predicted by rotating infall theory
● Jets of AGNs are probably similar phenomena
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Jets and Outflows
Questions:
● Launching process
● Contribution to angular momentum removal
● Relation between jet and outflows
● Confinement
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Basic picture
Jet: ● extremely collimated, high velocity flow● away from center of collapse, perpendicular to disk● evolution complementary to disk evolution
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Basic picture
Combination of jet and molecular outflow:
● Multiple velocity components
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Observations
Line shape tracing wind:
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Geometry and confinement
Dullemond (2010)
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Magnetic field winding - confinement
C. Fendt
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Magnetic field winding - confinement
j=c4
∇×B
f =1cj×B
● Right-hand rule: force points inwards
C. Fendt
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Hydrodynamic confinement of jets
• Jets are surrounded by cocoon of pressurized gas– Cocoon partly made of old jet material, partly by
swept up material from the environment– Jet material moves supersonically
● Shock only reduces the velocity compon-ent perpendicular to shock front. Therefore obliquely shocked gas is deflected toward the shock plane.
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Hydrodynamic confinement in jet:
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Hydrodynamic confinement of jets
• Head of jet (‘hot spot’) drills through ISM• Shocks seen as knots (Herbig-Haro objects)
Observed knot movement (HH30)
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Molecular flows: entrainment
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Velocity nesting: gas with higher velocity is more collimated, lower velocity outflow is more extended
Position-velocity diagrams:
The extremely high-velocity molecular outflow in IRAS 20126+4104 (Lebrón et al. 2006)
Molecular flows: observation
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Jet simulations
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Launching processes?
Correlation between mass outflow and accretion:
● Jet masses traced by excited lines of ionized gas
● Accretion in protostellar phase measured by total luminosity (up to 10-3 M⊙/yr)
Cabrit et al. 1990
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Launching processes?
Correlation between mass outflow and accretion:
Molecular outflow mass Outflow rate
→ close relation between accretion and outflow generation
→ favors some MHD jet launching mechanism
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Jet formation
X-wind model ↔ Disk-wind model
Two competing theories:
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Magnetospheric accretion
disk≈starInner disk boundary:
Corotation radius r co= GM star2
1/3
Alfvén radius ri
● Gas is loaded onto magnetic field lines (disk is des-troyed) where magnetic pressure = dynamic pressure.
Königl (1991)
● Magnetic coupling be-tween disk and star● Accretion along the field lines
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“X”-wind
In the X-wind model the magnetic field of a young star interacts with the magnetic field of the circumstellar disk to produce a gap between the star and disk. As gas spirals inward through the disk, it divides at the inner disk edge (the X-region) into two streams. A high angular momentum stream is flung away along the rotating magnetic field lines of the disk (the X-wind); the low angular momentum stream falls onto the star and helps build its mass.
X
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X-wind
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X-wind simulation
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Disk windSlingshot effect:Blandford & Payne (1982)
●Gravitational potential: =-GM
r 2z 2
=-GMr0 [ 12 rr0
2
r 0
r 2z 2 ]●Effective gravitational potential along field line (incl. sling-shot effect):
C. Fendt
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Disk wind
Infall Outflow
Critical angle:
60 degrees with disk plane.
Beyond that: outflow of matter.
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Disk wind model
Consistent with FU Orionis out-bursts
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Outflow size vs. distance
Ray et al. 2006, PPV
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X-wind versus Disk-wind
The X-wind model, the magnetic field of the star connects to the disk at the X-point. Here the accretion disk and star co-rotate and a wind, later collimated into a jet, is launched outwards along the open field lines.
The disk-wind model, the wind is launched along the open field lines of the disk over a range of radii down to the co-rotation radius.
http://www.jetsets.org/collimationofjets.html
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Arce et al. 2006, PPV
Different outflow models
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Are jets really a way to get rid of angular momentum?
Detection of jet rotation!
Bacciotti et al. 2002
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Observational constraints
• Foot-print radius: undecided – some observations claim very small ones (down to 0.014 AU = 3 R⊙ - would favor X-wind)
• Angular momentum of jet seems to be small – takes care of angular momentum problem of star, but disk has to look after itself
• Radial velocities and proper motions: 100-200 km/s for jets
→ Higher angular resolution needed to see deteching radius