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Sequentially Triggered Star Formation in OB Associations

Sequentially Triggered Star Formation in OB Associations. Thomas Preibisch & Hans Zinnecker. Max-Planck-Institute for Radioastronomy, Bonn, Germany. Astrophysical Institute Potsdam, Germany. ISO. r Oph cloud. age <= 1 Myr generation III. Upper Scorpius.

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Sequentially Triggered Star Formation in OB Associations

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  1. Sequentially Triggered Star Formationin OB Associations Thomas Preibisch & Hans Zinnecker Max-Planck-Institute for Radioastronomy, Bonn, Germany Astrophysical Institute Potsdam, Germany ISO r Oph cloud age <= 1 Myr generation III Upper Scorpius age = 5 Myr generation II Upper Centaurus - Lupus age = 17 Myr generation I

  2. Sco OB 2 Per OB 2 Ori OB 1 OB associations: (Ambartsumian 1947) - Unbound stellar groups containing O–B2 stars, Ø ~ 20 ... 50 pc - Density < 0.1 M pc-3 unstable against galactic tidal forces  < 30 Myr old Blaauw (1964, 1991): Many OB associations consist of distinct sub-groups with different ages  sequential (triggered ?) formation Summary of recent results on OB associations: Protostars and Planets V chapter by Briceno et al. (2006; astro-ph/0602446)

  3. Many observations show star formation near massive stars: YSOs O star OB stars  RCW 79 blue: Ha, red: 8 mm Zavagno et al. (2006, A&A 446,171) Trifid Nebula HST, Hester et al. (1999) YSOs Star formation in irradiated globules: "radiatively driven implosion" Star formation in swept-up shells: "collect & collapse" model Q: Was the formation of the YSOs triggered, or did YSOs form prior to the arrival of the shock waves ? A: Determine ages of the YSOs and compare to shock arrival time OB associations show the result of a recently completed star formation process, star formation history and initial mass function allow a quantitativecomparison to models

  4. Theoretical models for triggering mechanisms in OB associations: 1. Sequentially triggered formation of OB subgroups (Elmegreen & Lada 1977, Lada 1987) Predictions: -Bimodal star formation: low-mass stars form independently  are on average older, show large age spread - IMF variations: younger OB subgroups should have larger fractions of low-mass stars         star formation terminated          Age spread among low-mass stars: [8....12] Myr [4....12] Myr [0....12] Myr IMF variations:defict excess of low-mass stars

  5. Theoretical models for triggering mechanisms in OB associations: 2. Radiation-driven implosion of globules near OB stars (Bertoldi 1989; Lefloch & Lazareff 1994; Kessel-Deynet & Burkert 2003) Predictions: - OB stars form first, are older than low mass stars - Age gradients: stars close to the O star are older than those further away (see also next talk by W.P. Chen) Hester & Desh (2005)     Ages of the low-mass stars: 7 , 5 , 3 , 1 Myr

  6. Theoretical models for triggering mechanisms in OB associations: 3. Supernova shock wave compression of cloud (e.g. Foster & Boss 1996, ApJ 468, 784; Vanhalla & Cameron 1998, ApJ 508, 291) At suitable distances of ~ 20 ... 100 pc, where vshock = 20 ... 50 km/sec, cloud collapse can be triggered by supernova shock waves Predictions: - High- and low-mass stars have same age - Small age spread (since vshock > 20 km/sec) - Age difference of ~ 5...10 Myr between subgroups NEXT: Predictions versus observations

  7. The nearest OB association: Scorpius - Centaurus (Sco OB2) Hipparcos revealed B to F stars de Zeeuw et al (1999, AJ 117, 354) de Bruijne (1999, MNRAS 310, 585) D= 144 pc 49 B-stars Upper Scorpius D = 142 pc 66 B-stars Upper Centaurus - Lupus D = 116 pc 42 B-stars Lower Centaurus - Crux a Sco 25 pc 10

  8. The nearest OB association: Scorpius - Centaurus (Sco OB2) Mamajek et al.(2002, AJ 124,1670) Ages of the massive stars from MS turnoff t = 5 Myr Upper Scorpius t = 17 Myr Upper Centaurus - Lupus t = 16 Myr Lower Centaurus - Crux a Sco 25 pc 10 What about the low-mass stars ? de Geus et al. (1989, A&A 216,44)

  9. The stellar population of Upper Scorpius Huge field star confusion in extended OB associations: Younglow-mass members must be individually identified by spectroscopy (6708Å Lithium lines) - X-ray selected candidates: Walter et al (1994, AJ 107,692) Preibisch et al(1998, A&A 333,619) - Survey with multi-object spectrograph 2dF: Preibisch et al (2002 AJ 124, 404):  250 low-mass members (representative sample) Upper Scorpius a Sco 25 pc + 114 higher-mass stars from Hipparcos:  364 known members SpT = B0.5 ... M6 , M = 20 M ...0.1 M 10 Statistically robust & well defined sample Individual spectral types and extinctions known: derive IMF and star formation history from HRD

  10. HR Diagram for Upper Sco 5 Myr isochrone High- mass and low-mass stars are coeval Spread of isochronal ages Preibisch et al (2002, AJ 124, 404) Reasons for spread of isochronal ages: - distance spread: D D / D = 30 pc / 145 pc ~ ± 0.25 mag - unresolved binaries: <~ + 0.75 mag - photometric variability <~ ± 0.3 mag HRD consistent withno age spread, Dt < 1-2 Myr - Mass functionisconsistent with field star IMF

  11. Implications on the star formation process age of the high-mass stars: 5 Myr diameter: ~ 30 pc age of the low-mass stars: 5 Myr 1D velocity dispersion: 1.3 km/sec age spread < 1-2 Myr  lateral crossing time ~ 25 Myr age spread << crossing time external agent coordinated onset of star formation over the full spatial extent ScoCen is surrounded by several H I shells De Geus (1992, A&A 262, 258): Wind & supernova driven expanding superbubble from UCL crossed Upper Sco ~ 5 Myr ago De Geus (1992, A&A 262, 258)

  12. Scenario for the star formation history de Geus (1992, A&A 262, 258); Preibisch & Zinnecker (1999, AJ 117, 2381) Supernova & wind driven shock wave from UCL crosses USco cloud Wind & ionizing radiation of the massive stars disperse the cloud Supernova in USco star formation terminated cloud fully dispersed star formation triggered star formation in r Oph triggered Supernova & wind driven shock wave from USco reaches r Oph cloud

  13. Scenario for the star formation history de Geus (1992, A&A 262, 258); Preibisch & Zinnecker (1999, AJ 117, 2381) Supernova & wind driven shock wave from UCL crosses USco cloud Wind & ionizing radiation of the massive stars disperse the cloud Supernova in USco star formation terminated cloud fully dispersed star formation triggered "Any theory of star formation is incomplete without a corresponding theory of cloud formation" (Elmegreen & Lada 1977) Hartmann et al (2001, ApJ 562,852) and others: Molecular clouds are short-lived structures, i.e.do not exist for > 10 Myr without forming stars and "wait for a trigger" star formation in r Oph triggered Supernova & wind driven shock wave from USco reaches r Oph cloud

  14. Rapid formation of molecular clouds and stars Ballesteros-Paredes et al.(1999, ApJ 527,285); Hartmann et al.(2001 ApJ 562, 852); Clark et al.(2005, MNRAS 359,809) Large-scale flows in the ISM accumulate and compress gas to form transient molecular clouds Wind & supernova shocks waves create coherent large-scale velocity fields,  formation of large structures in which star formation can be triggered nearly simultaneously Ballesteros-Paredes et al. (1999, ApJ 527,285) Hartmann et al. (2001 ApJ 562, 852)

  15.       Triggered cloud & star formation in ScoCen T = - 14 Myr OB star winds in UCL create expanding superbubble (v ~ 5 km/sec) Interaction with ISM flows starts to sweep up clouds UCL 30 pc

  16.       UCL 60 pc Triggered cloud & star formation in ScoCen T = - 5 Myr After supernovae in UCL added energy & momentum to the expanding superbubble, the shock wave (~ 30 km/sec) crossed the USco cloud, increased pressure triggered star formation in USco

  17. Triggered cloud & star formation in ScoCen T = - 1 Myr Shock wave from USco superbubble triggers star formation in r Oph and Lupus I clouds Lupus I cloud generation III r Ophiuchus generation III Upper Scorpius generation II Upper Centaurus - Lupus generation I

  18. + Centroid space motion in the rest-frame of UCL Model versus observations Model Predictions I: Stellar groups triggered in swept-up clouds move away from the trigger source Hipparcos proper motions of USco and UCL members Observation: Determination of centroid space motions of the groups: de Bruijne (1999, MNRAS 310, 585)  Upper Sco moves away from UCL with v ~ 5 (±3) km/sec de Zeeuw et al (1999, AJ 117, 354)

  19. T = 0 (today) CrA 0 TW Hya Y (pc) -50 UCL -100 hCha 0 50 100 150 Model versus observations Model Predictions I: Stellar groups triggered in swept-up clouds move away from the trigger source Observation: Mamajek & Feigelson (2001) Several young stellar groups: - h Cha cluster - TW Hydra Association - CrA cloud move away from UCL with v ~ 10 km/sec were located near the edge of UCL 12 Myr ago (when SN exploded) T = - 12 Myr 0 Y (pc) -50 UCL -100 0 50 100 150 X (pc) X (pc) adapted from: Mamajek & Feigelson (2001,in: Young Stars Near Earth, ASP 244, p. 104; astro-ph/0105290)

  20. Model versus observations S Model Predictions II: Elongated star forming clouds form at the intersection of two expanding flows Observation: Lupus I cloud located at interface of USco and UCL (post-SN, wind-driven) superbubbles       USco UCL                       Dust extinction map from Dobashi et al. 2005, PASJ 57,S1

  21. How general are these findings? Several OB associations showsubgroupsequences of three generations that provide evidence for triggered formation, e.g. ScoCen: UCL  USco  r Oph / Lupus I Cep OB2: NGC 7160  IC 1396  VDB 142 Superbubbles in W3/W4 (Oey et al. 2005, AJ 129, 393) BUT: Some associations also contain subgroups with similar ages e.g.:ScoCen: UCL [17 Myr] - LCC [16 Myr]

  22. Extragalactic example of supernova triggering in OB associations: Hen 206 (LMC) Gorjian et al. (2004,ApJS 154, 275) OB association NGC 2018: age ~ 10 Myr Supernova-driven expanding H I shell v = 22 km/sec 80 pc optical image Spitzer image blue: 3.6+4.5 mm, cyan: 5.8 mm, green: 8.0 mm, red: 24 mm Triggered formation of several new OB subgroups Explanation for subgroups with the same age (e.g., ScoCen: UCL [17 Myr] - LCC [16 Myr] )

  23. How general are these findings? Results for well investigated OB associations:(Sco OB2, Cep OB2, Ori OB1) Briceno et al. (2006; Protostars & Planets V chapter; astro-ph/0602446) -IMF of most OB subgroups consistent with field IMF, no goodevidence for IMF variations -Low- and high mass stars have the same ages, have formed together - In most regions, age spreads are (much) smallerthan the crossing time  consistent with models of large-scale triggering by shock waves Supernova (+wind) driven shock waves play an important role, but other triggering mechanisms are also at work in some regions:

  24. Sicilia-Aguilar et al (2004, AJ 128, 805; 2005 AJ 130, 188) Reach et al (2004, ApJS 154, 385) Cep OB 2 association: IRAS 12 mm 1 13 pc NGC 7160 (10 Myr) VDB 142: Radiation-driven implosion of globule (no supernova triggering!) The globule will form a small stellar group, but no OB subgroup! IC 1396 (4 Myr) <1 Myr VDB 142 class 0 / class I protostars Spitzer 3.6+4.5 mm, 5.8+8 mm, 24 mm Reach et al (2004, ApJS 154, 385) HD 206267 (O6)

  25. Conclusions: OB subgroups with well defined age sequences and small internal age spreads suggest large-scale triggered formation scenarios. (Supernova/wind driven shock waves) Expanding bubbles coherent large-scale ISM flows  new clouds Supernova shock waves cloud compression  triggered formationof whole OB subgroups (several 1000 stars). Other triggering mechanisms (e.g. radiation-driven implosion of globules) may operate simultaneously, but seem to form only small groups of stars (i.e. are secondary processes). Note: Our Sun formed in an OB association ! Supernova shock wave injected short-lived radionucleids (e.g. 26Al). (Cameron & Truran 1977; Hester & Desh 2005)

  26. THE END

  27. Interpretation of the HR Diagram: Age spread or no age spread ?? Coeval population of 5 Myr old stars Perfect world: no errors, no uncertainties simulated HRD age histogram

  28. center: 145 pc  Upper Sco front: 130 pc back: 160 pc Interpretation of the HR Diagram: Age spread or no age spread ?? Coeval population of 5 Myr old stars Perfect world: no errors, no uncertainties simulated HRD Reality: - photometric variability & errors - unresolved binaries - spread of individual distances age histogram  false impression of a large age spread and an accelerating star formation rate in an actually perfectly coeval population ! Analysis for Upper Sco: no detectable age spread, t = 5 Myr (±1-2 Myr)

  29. Age sequences / spreads and projection effects                 no observed age sequence false impression of a large age spread 1 ... 15 Myr line-of-sight 15 Myr 1 Myr 5 Myr e.g. Orion Nebula Cluster: To Earth simulated side-view: Ori OB 1C members ? (~ 5 Myr) Distributed T Tauri stars: ~ 2 -10 Myr Trapezium cluster stars: ~ 1 Myr BN complex, OMC-S protostars: <~ 0.1 Myr O'Dell 2001 ARAA 39, 99

  30. N The Supergiant Shell Region in IC 2574 Cannon et al. (2005, ApJ 630, L37) Stewart & Walter (2000, AJ 120,1794) N cavity surrounded by expanding shell Ø ~ 800 pc, M ~ 106 M v ~ 25 km/sec central OB association total mass ~150 000 M age: ~ 11 Myr young OB associations M ~ 5000 ... 300000 M ages ~ 1 ... 4 Myr U + V + I Expanding shell triggers a second generation of OB associations on its rim

  31. The Superbubble LMC4 Yamaguchi et al. (2001, ApJ 553, L185) Note: most massive clouds are at bubble intersection shell diameter 1.9 kpc v(exp) = 10 – 40 km/sec center: 400 OB stars ages 9-16 Myr stars at the rim are < 6 Myr Ha image, green contours: CO open circles: > 10 Myr clusters, filled circles: < 10 Myr old clusters

  32. "Pillars of Creation" in the Eagle Nebula (M16) VLT near-infrared image; McCaughrean & Andersen (2002) Only 11 of 73 EGGs have YSOs < 100 stars will eventually form in the pillars, much less than the stellar population of the exciting OB cluster NGC 6611 HST optical image; Hester et al. (1996) Detection of evaporating gaseous globules "EGGs"; sites of triggered star formation ?

  33. Triggered massive star formation in RCW 79 Zavagno et al. (2006, A&A 446,171): blue: Ha, red: Spitzer 8 mm central OB cluster, including an O4 star (~60 M) Radius of HII region = 6.4 pc for n ~ 2000 cm-3 tdyn = 1.7 Myr collected layer fragmented ~105 yr ago, consistent with ages of YSOs Data consistent with "collect & collapse model" fragmentation of the shocked dense layer around an expanding HII region Whitworth et al (1994) compact HII region, ionized by an O9 star (~20 M), contains many class I protostars

  34. 30 Dor– NGC 2070 ( 40 O3 stars, 60 000 M , age = 2-3 Myr ) 1' 15 pc Radiation of the massive stars in the central cluster triggers star formation in the nebular filaments (Rubio et al. 1998) "Two stage starburst"

  35. 2 16 pc lOri association l Ori (O8) + 60 B-type stars, ~ 6 Myr IRAS12+24+100 mm Dolan & Mathieu(2001, AJ 121, 2124) Dolan & Mathieu (2002, AJ 123, 387) -global IMF consistent with field IMF - low-mass stars concentrate - near l Ori, ages ~ 1 – 6 Myr no ongoing star formation, age spread probably real - near the dark clouds B30+B35 continuing star formation, ages ~ 0 - 6 Myr B30 l Ori B35 Star formation history: 1 Myr ago, a supernova explosion terminated the star formation process near the center, but there is still ongoing star formation in the dark clouds B30 and B35 star formation begins

  36. NGC 604(in M33) Maiz-Apellaniz et al. (2004, AJ 128,1196) 200 OB stars, age ~ 3 Myr Rcavity = 60 pc

  37. Superbubbles in W3/W4 Oey et al. (2005, AJ 129,393) W3 North: 105 yr "230 pc shell" age ~ 6 – 10 Myr W3 IC 1795: 3-5 Myr W3 Main: 105 yr W3 OH: 105 yr IC 1805: 1-3 Myr W4

  38. Upper Sco UCL Model versus observations Model Predictions I: swept-up clouds should be elongated along the direction of the shock front Observation: Initial configuration for Upper Sco: from proper-motion back-tracing,Blaauw (1991) elongation as signature of a swept up cloud                

  39. Ori OB 1 association Briceño et al (2005, AJ 129, 907) identify 197 low-mass members of Ori OB 1a and 1b derived ages: 1a: ~10 Myr, 1b: ~5 Myr  High- and low-mass stars are coeval 2 16 pc 1a (~ 10 Myr) 1b (~ 3 Myr) 1c (~ 4 Myr) 1d (= ONC) Ages of the OB stars from Brown et al (1994, A&A 289, 101)

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