Jets from Young Stars
John Bally
Center for Astrobiology Center for Astrophysics and Space Astronomy Department of Astrophysical and Planetary Sciences University of Colorado, Boulder
Outline:
• Jets & Herbig Haro Objects
• • • • •
Relation to Molecular Outflows Giant Outflows Irradiated Jets & Microjets Massive Star Outflows Impacts: Self-Regulation of star formation Turbulence generation Cloud disruption • Launch & Collimation
HH 212 H2 (Mc Caughrean & Zinnecker VLT)
HH 46/47: Ha [SII] [OII]
Spitzer IRAC:
3 – 8 mm
HH 46/47 (Hartigan et al. 05, AJ BR06)
HST 1994
HH 46/47 (Hartigan et al. 05, AJ BR06)
HST 1997
Outflows:
Jets, Winds => Wide-Angle Cavities
Disk winds X-winds Internal working surfaces Terminal working surface
HH jet (high V) HI CO outflow (low V) H2 (moderate V)
L1551
(BR06)
HH 30 (HST)
X-ray source ~0.5” from IRS5
Ha [SII]
CO J=2-1
L1551
CO J=2-1
6-7 km/s
8-12 km/s
1-5 km/s
Jets from Young Stellar Objects (YSOs)
• Tracers: 106 K plasma X-ray Ha, [SII], [NII], [OI], [OIII] visual [FeII], H2 infrared CO, HCO+, SiO mm free-free, non-thermal, masers cm • Manifestations of outflows: Visual jets, micro-jets (jet beam) Herbig-Haro objects & NIR (H2) shocks Molecular outflows (swept-up/entrained) • dM/dt decrease with evolutionary stage Class 0: > 10-5 Solar masses/year Class I: 10-6 Solar masses/year Class II/II: 10-7 10-9 Solar masses/year • Velocity Increase with evolutionary stage
Jets from Young Stellar Objects (YSOs)
• dM /dt increases as L0.8 • V increases as L0.2 Acceleration Mechanisms: - Radiation pressure ? NO - L/c too low - Thermal pressure gradient? NO - too low - MHD YES! Uchida-Shibata, Lovelace – helical torsion, impulsive Pudritz-Norman disk wind - advected B, steady Shu X-wind - stellar dynamo, steady - Dynamical decay; release of gravitational potential (Orion) Collimation: - Magnetic hoop stress - Ambient density gradient - Ram-pressure of infalling envelope
HH 3 NGC 1999 New jet
HH 1
HH 2
proplyd
HH 2
HH 1
HST 1997 - 1994
HH 2
HH 1
HST 1997 - 1994
HH 1 jet
HST 1997 - 1994
HH 1 jet
HST 1997 - 1994
HH 1
HST 1997 - 1994
HH 1
HST 1997 - 1994
HH 2: Small scale chaotic motion (102 - 104 AU)
HST / WFPC2 1994
(Bally et al. 2000; BR06)
HH 2: Small scale chaotic motion (102 - 104 AU)
HST / WFPC2 1997
(Bally et al. 2000; BR06)
NGC 1333
IC 348
Miesch & Bally (94); BR06
IRAS 03235+3004
NGC 1333
Ha, [SII] Walawender, Bally, Reipurth (06) Spitzer/IRAC Jorgensen et. (06)
Giant Outflows
• Symmetries: C-shaped: ejection of star, wind interactions S-shaped: outfow orientation change • Fossil record of Mass Loss (accretion) history
• Source of cloud turbulence
• Chemical Rejuvenation, CI, C+ in ICM (inter cloud medium)
• Origin of Cloud Internal Structure (shells, holes: cf. Circinus) Structure + UV => Turbulence • Major eruptions of YSO every few thousand years ejecta decelerates, blows out of cores • Non-linear Evolution of Instabilities: cooling => structure
HH 34
HST 1997 - 1994
HH 34
HST 1997 - 1994
HH 34 parsec-scale flow
2.5 pc
HH flows attain pc-scales
HH92 in Orion B CTIO 4m MOSAIC
HH flows attain pc-scales
HH 131
Orion A: - Outflows up to 30 pc long !
M42
HH 131
HH 1/2
Cepheus A: L ~ 2 x 104 Lo
CO CO CO
DV = 10 km/s
DV = 6 km/s
H2
DV = 4 km/s
Ceph A East
Ceph A West
Cepheus A: L ~ 2 x 104 Lo
Ha [S II] H2 Hartigan et al.
Cepheus A: L ~ 2 x 104 Lo
Near-IR
East
X-ray
Ha
West
X-ray
X-ray
Pravdo & Tsuboi 05
Ceph A
Cunningham, Moeckel, & Bally
Ceph A
N. Patel (05)
Cunningham, Moeckel, & Bally
Ceph A precessing jet: P ~ 2 x 103 yr ? Cunningham, Moeckel, & Bally
Orion Nebula
OMC1
HH 202
HH529
HH269
OMC1-S
HH 203 HH 204
Orion Nebula
OMC1
HH 202
HH529
HH269
OMC1-S
HH 203 HH 204
q 1C
LV 5
HH202 jet
HH514
HH202 source
HH202 source
OMC1-S
HH529
q 1C
LV 5
11.7 mm TReCS
HH202 jet
HH514
HH202 source
HH202 source
OMC1-S
HH529
Zapata et al. (2005)
Zapata et al. (2006)
0.5 – 2.2 mm 104 AU
11.7 mm 104 AU
Orion BN/KL H2 fingers E ~ 1048 erg
Dynamical Decay of Sub-cluster of massive stars
~ 500 years ago
(N. Cuningham 2006 PhD thesis)
Nathaniel Cunnigham PhD (2006)
H2 Proper Motions
Nathaniel Cunnigham PhD (2006)
t = r/v ~ 500 yr
t = 1,000 yr
N. Cunningham, J. Bally, M. Burton, M. Hayashi (in prep)
High-velocity stars: I , BN , n (Gomez et al. 2005)
BN: V~ 30 km s-1
I: ~ 13 km s-1
n: ~ 20 km s-1
OMC1 H2 fingers
Kaifu et al. (00); Underhill et al (01)
The Magnetic Bomb
• ~105 to 500 year ago:
- Velocity damping + orbit decay - 200 AU sub-cluster of 4+ massive stars in OMC1 - Shear dynamo: ~10 mG B field => ~ 40 G in 105 years: EB ~ 1048 ergs - Dynamical decay of non-hierarchical system: E* ~ 3x1047 erg - Ejection of high velocity stars (BN, I, n) => ~ V* ~ 20 km/s Eout ~ 3x1047 erg - Disruption of magnetized circumstellar disks: Vfast ~ 500 km/s
• 500 years ago:
=> Explosive, wide-angle outflow!
Irradiated Jets
• Nearby OB stars photo-evaoprate cores s Ori (HH 444, 445, 446); Orion Nebula (Bally 06) • Asymmetries: Brighter jet - slow Fainter jet - fast Mass loading of fast beam • Lyman continuum: determine n, V, P, E independent of nonlinear shock physics • Irradiated micro-jets from Orions proplyds dM/dt ~ 10-9 Mo low V ( few Myr old star)
STIS
Devine et al. 01
HH 514 micro-jet in Orion: Ha, [HII]
(HST/STIS)
LL Orionis: wind-wind collision fronts – jet driven!
HH502 in Orion: C-symmetric jet-sidewind collision
HH400 rim
Crossing flow
Redshitfted bows
Proplyd & jet
To q1C
Blueshifted bow & jet cocoon
HH505 in Orion: jet-sidewind collision fronts
d253-535 in M43
The Carina Nebula (CTIO Schmidt)
The Carina Nebula
Mosaic: CTIO 4m
ACS: HST
Irradiated jets in h Car (Tr 14):
Nathan Smith et al. (in prep)
Irradiated jets in h Car (Tr 14):
Nathan Smith et al. (in prep)
HH 666
120 arcsec
[O III] Ha [S II]
HH 666
30 arcsec
[O III] Ha [S II]
HH 666
[O III] Ha [S II]
HH 666
Ha
[S II]
JHK
HH 666
HH 666 IRS
Class I YSO
Pab [Fe II] H2
Jet Symmetries:
• S – shaped: - Precession • Z – shaped: - Eccentric binary - Close-passage of sibling star • C-shaped: - Jet in a sidewind - Motion of source (ejection from cluster) • Monopolar (one-sided) - Obscuration - Mass loading
Variability:
dM/dt V orientation degree of collimation
The Engine
Accretion + Spin => Outflow • Protostar Convection + Rotation: Stellar Dynamo • Disk Rotation: Shear Dynamo
MHD Winds (M 5 Solar masses) • Dynamical Decay • Radiation Pressure, Ionization
The future:
- SOFIA: 2.5 m @ 41,000 ft in a 747, High R
FLITECAM, FORCAST, EXES, FIFI LS, GREAT, CASIMIR R ~ 300 - 107
-
HST (ACS + WFPC 3) E-VLA ALMA JWST
Conclusions :
• Jets – Sources of turbulence, - Ionization - Cloud rejuvenation • MHD launch /collimation? - Repetitive accretion events & Uchida-Shibata bursts? - Advected disk winds? - Dynamo generated X-winds? • Massive YSOs: - Radiation pressure - Dynamical interactions? YSO jets resemble: - AGN/quasars (massive black-holes) - micro-quasars (stellar mass BHs) - PN, SN, symbiotic stars
OMC1 - 12 mm
(Shuping et al. 2004)
NH3
H2O masers
Radio sources
OMC1 (Shuping et al. 2004)
NH3
OMC1 SiO J=1-0 (Greenhill et al. 2004)
OMC1 SiO J=1-0 & 7mm continuum (Greenhill et al. 2004)
OMC1 SiO J=1-0 (Greenhill et al. 2004)
OMC1 H2 fingers
Orbit Decay:
Massive stars orbiting in r-2 sphere of gas + stars
Nick Moeckel PhD Thesis (CU Boulder, in preparation)
Flow Properties
Parameter (M5 Solar) 100 - 1,000 10-5 to 10-2 unit km/s Mo yr-1 • Wind/jet velocity 100 - 1,000 • dM/dt 10-5 to 10-9
• M(H2)
• t • Size: • E
0.001 to 10
104 (Class 0) 105 (Class I) 106 (>Class II) 1 to 10 1043 to 1047
1 to 3,000
104 to 105
Mo
yr yr yr pc erg
1 to 20 1046 to 1050
• Lmech
10-0 to 10-3
10-1 to 103
Lo