Out Outflo lows ws f from Yo Young S ung Stars: Fr From Jets to Expl plosive Fe Feedb dbac ack In In Sta tar Forma mati tion Jo John Ba Bally 1 1 Ce Cente ter for As Astr troph physics and d Spa pace As Astr tronomy my (CAS CASA) A) Dep Department ent o of A Astrophy hysical a and nd Pl Planet netary S Scienc ences es ( (APS PS) Un University of Colorado, Boulder
L1551 L1 H a [S [SII] HL HL & XZ Ta Tau HH HH 30 IR IRS5
Ac Accretion + Spi pin + Magnetic Fields ds (o (or radiation) Outf Ou tflo low - Fo Fossil il re record rd of ac accre retio ion his istory ry, , N-bo body dynam amic ics - Fe Feedbac back Impac act in in Self lf-Re Regulation on (Co Coup uple P, P, E E, d directl tly i into nto p parent c nt cloud ud) - Mos Most (all ?) YSO SOs have ve them (a (all accreting, sp spinning, magnetized syst systems? s?) )
Som Some Prob oblems in St Star For ormation on St Star for ormati tion on – a a fundam amental al cosm smic process: ss: Det Deter ermines es the e co cosmic c ev evolution of baryons IM IMF => => massive stars rs => => nuc nucleo-sy synthesi sis s => elemental al enrichment => => planet form rmation => => life … - Wh What determines s st stellar masse sses s and the IMF? In Initial Conditions ? Feedback? N-bo body dynamic ics? - Wh Why y is s the Star Formation Effi fficiency y (S (SFE) ) so so low? w? Tu Turbulence? B B ? Feedback ? - Wh What det eter ermi mines es the e St Star For ormation on Ra Rate (SF SFR) R) ? Ex Exter ernal or inter ernal proces cesses es ? Ne Nearby s star f formation ( n (e.g. M Milky W Way) i ins nsight hts t to c cosmic da dawn (J (JWS WST T Science)
Se Self lf-Re Regu gula lation ion in in St Star Fo Format ation Wh What st stops s ac accre retio ion, , sets M * , , & & th the IM IMF? Fe Feedbac back + + N-bo body dy dynami mics cs ? The The “ Fe Feedbac back Lad adder ” Pr Progression o n of e eve ver s strong nger f feedb dback i impa pacts Protostar O Pr Out utflows = = > > lo local, , low M * , , coupl ples di dire rectly to cloud FUV/heat FU ating => EU EUV/ionization => St Stellar winds => Ra Radiati tion on pressure => M. M.S. dynami mic interactions / / me mergers => Po Post-M. M.S. outflows => SN SNe => glo globa bal, , high M * Bl Black holes Fe Feedbac back fa failur ure => => High igh SF SFE, bo bound clu luste ters rs?
Pr Protostella llar Out Outflo low F Feedba back: k: <V(H a )> <V(CO)> <V > ~1 ~1–10 10 km/s <V <V(H 2 )> )> ~10–100 100 km/s <V )> >30 – 500 500 km/s
Pa Parsec-sca scale e flows s from Class ss 0 YSOs 8 µ m 5 µ m HH HH 212 (Orion on B) 4. 4.5 m (H 2 ), , 8 m 1 pc NORTH HH 212 Source 8 µ m 5 µ m HH HH 91/9 /92 (Orion on B) 4. 4.5 m (H 2 ), , 8 m (note e du dust st sh shel ell !) 1 pc NORTH HH 91/92 Source
[ O II II ] Ha Ha [ S II II ] = 0.38, 0.65, 0.67 µ m HH 4 HH 46/47 NT NTT
, 8 µ m HH 4 HH 46/47 S Spitzer H 2 PAH PAH 3. 3.6, , 4. 4.5, (N (Noriega-Cr Cres espo+ + 04) 04)
HH HH 46/4 /47 CO CO CO CO (A (ALMA), , [S [SII] ] (H (HST) T) (Ar Arce ce+ + 2013) 2013)
HH HH 46/4 /47 (H (Hartigan et al. 05, AJ) V PM PM ~ ~ 300 300 km/s HST HST 1994
HH HH 46/4 /47 (Ha Hartigan et et al. 05, AJ AJ) V PM PM ~ ~ 300 300 km/s HST HST 1997
HH HH 46/4 /47 H a CO CO c conf nfine ned to to <10% <10% o of S Size & & V Velocity ty ! ! (S (Stan anke, , McCau augrean an, , & Zinnecker 1999)
Or Orion ion A CO CO 1 1-0 0 T pe peak CA CARMAOrion (K (Kong S. S. et al. . 2018) [SII] CT CTIO 4m 4m
Or Orio ion OM n OMC1: CO 1 CO 1-0 N-bo body dynam amic ics in in dense gas gas => => Orbit Orbit decay ay V = V = 4 4 – 12 12 km/s Ko Kong S. S. et t al.2 .2018 => => N-bo body dynam amic ics: : im importan rtant t for r IMF
=> => Novae, ste tella llar r merge rgers rs, SNe, Pro roto toste tella llar r merge rgers rs? CO CO 1 1-0 V = V = 4 4 – 12 12 km/s Ko Kong S. S. et t al.2 .2018
=> => Novae, ste tella llar r merge rgers rs, SNe, Pro roto toste tella llar r merge rgers rs? CO CO 1 1-0 V = V = 4 4 – 12 12 km/s Ko Kong S. S. et t al.2 .2018
=> => Novae, ste tella llar r merge rgers rs, SNe, Pro roto toste tella llar r merge rgers rs? CO CO 1 1-0 V = V = 4 4 – 12 12 km/s Ko Kong S. S. et t al.2 .2018
? CO CO 1 1-0 V = V = 4 4 – 12 12 km/s Ko Kong S. S. et t al.2 .2018
Ho How ? CO CO 1 1-0 V = V = 4 4 – 12 12 km/s Ko Kong S. S. et t al.2 .2018
Or Orion ion A CO CO 1 1-0 0 T pe peak CA CARMAOrion (K (Kong S. S. et al. . 2018) [SII] CT CTIO 4m 4m
Ho How Common are Explosive ve Outfl flows?: Outf Ou tflo lows Se Seve veral `fos ossil’ Galactic candidates exist CO CO 1 1-0 ~10 3 ye ~ is ~ isotro tropic ic for r ~10 years bipolar bip lar on lo longe ger r tim times (e.g. .g. DR 21) 21) 2.6 2. 6 mm => => Few % of known (massiv ive-st star) ) outflows ws Lumino Lum inous us E Extra-Ga Galactic IR-tr transients ts ~150 IR-on ~150 only transients in ~20 nearby star-fo forming ng galax galaxie ies 5 µ m 3. 3.6 6 & 4. 4.5 m Spi pitzer er SPIRITS Sources ces (Ka Kaslilwal+ + 2017) 2017) => => Novae, ste tella llar r merge rgers rs, SNe, Pro roto toste tella llar r merge rgers rs?
Ho How Common are Explosive ve Outfl flows?: Outf Ou tflo lows Seve Se veral `fos ossil’ Galactic candidates exist [SII] [S ~10 3 ye ~ ~ is isotro tropic ic for r ~10 years bip bipolar lar on lo longe ger r tim times (e.g. .g. DR 21) 21) 6716/6731 6716/ 6731 A => => Few % of known (massiv ive-st star) ) outflows ws Lum Lumino inous us E Extra-Ga Galactic IR-tr transients ts ~150 ~150 IR-on only transients in ~20 nearby star-fo forming ng galax galaxie ies 5 µ m 3. 3.6 6 & 4. 4.5 m Spi pitzer er SPIRITS Sources ces (Ka Kaslilwal+ + 2017) 2017) => => Novae, ste tella llar r merge rgers rs, SNe, Pro roto toste tella llar r merge rgers rs?
HH HH 34 / 201 / 222 Ha Ha [S [S II II ] ] (Re Reipurth+ Su Subaru)
HH HH 34 / 201 / 222 Ha Ha [S [S II II ] ] (Re Reipurth+ Su Subaru)
Outflows ~150 YSOs in NGC 1333 H a , , [S [SII] Walawender, Bally, Wa y, Re Reipurth (06) Spitz Sp tzer/IRA RAC Jo Jorgensen et. (06)
NGC 1333 Ha, [SII] H 2
NGC 1333 8 µ m CO CO CARMA Plunkett+ (2013) 0.15 pc
G28.37+0.07 8 µ m CO CO ALMA Kong+ (2019)
• km s -1 yr -1 ) Low-Mass 10 -1 10 -2 Mechanical Force (M O 10 -3 Class 0 10 -4 10 -5 10 -6 Class I High-Mass 10 -7 10 -1 10 0 10 1 10 2 10 3 10 4 10 5 Source Luminosity (L O • ) Maud et al. (2015)
CARMAOrion 12 CO (Kong+ 2018) 5 7 9 km/s
CARMAOrion 12 CO (Kong+ 2018) 6 8 10 km/s
CARMAOrion 12 CO (Kong+ 2018) 7 9 11 km/s
CARMAOrion 12 CO (Kong+ 2018) 8 10 12 km/s
Ho How Common are Explosive ve Outfl flows?: Se Seve veral `fos ossil’ Galactic candidates exist ~10 3 ye ~ is ~ isotro tropic ic for r ~10 years bip bipolar lar on lo longe ger r tim times (e.g. .g. DR 21) 21) => => Few % of known (massiv ive-st star) ) outflows ws Lum Lumino inous us E Extra-Ga Galactic IR-tr transients ts ~150 IR-on ~150 only transients in ~20 nearby star-fo forming ng galax galaxie ies 5 µ m 3. 3.6 6 & 4. 4.5 m Spi pitzer er SPIRITS Sources ces (K (Kasl slilwa wal+ 2017) => => Novae, ste tella llar r merge rgers rs, SNe, Pro roto toste tella llar r merge rgers rs?
Ho How Common are Explosive ve Outfl flows?: Se Seve veral `fos ossil’ Galactic candidates exist ~10 3 ye ~ is ~ isotro tropic ic for r ~10 years bip bipolar lar on lo longe ger r tim times (e.g. .g. DR 21) 21) => => Few % of known (massiv ive-st star) ) outflows ws Lum Lumino inous us E Extra-Ga Galactic IR-tr transients ts ~150 IR-on ~150 only transients in ~20 nearby star-fo forming ng galax galaxie ies 5 µ m 3. 3.6 6 & 4. 4.5 m Spi pitzer er SPIRITS Sources ces (K (Kasl slilwa wal+ 2017) => => Novae, ste tella llar r merge rgers rs, SNe, Pro roto toste tella llar r merge rgers rs?
Pr Pre-ex expl plosion ca cavities es by by pre re-ex existing out utfl flows?
The The O Orion E n Explosion infrared (2 µ m) Nea Near-in m) Gemini-S Ge GS GSAOI + + GE GEMS (B (Bally y et al. 2015) )
1999 1999
2013 2013
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