Out Outflo lows ws f from Yo Young S ung Stars: Fr From Jets - - PowerPoint PPT Presentation

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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

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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 Bally1

1Ce

Cente ter for As Astr troph physics and d Spa pace As Astr tronomy my (CAS CASA) A) Dep Department ent o

  • f A

Astrophy hysical a and nd Pl Planet netary S Scienc ences es ( (APS PS) Un University of Colorado, Boulder

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SLIDE 2

HL HL & XZ Ta Tau HH HH 30 IR IRS5

L1 L1551

Ha [S [SII]

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SLIDE 3

Ac Accretion + Spi pin + Magnetic Fields ds

  • 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

  • n

(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?) )

Ou Outf tflo low

(o (or radiation)

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SLIDE 4

Som Some Prob

  • blems in St

Star For

  • rmation
  • n

St Star for

  • rmati

tion

  • n – 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

  • rmation
  • n 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)

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SLIDE 5

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 Pr Protostar O Out utflows = =>

> lo local, , low M*, , coupl ples di dire rectly to cloud

FU FUV/heat ating => EU EUV/ionization => St Stellar winds => Ra Radiati tion

  • n 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?

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SLIDE 6

Pr Protostella llar Out Outflo low F Feedba back: k:

<V <V(CO)> > ~1 ~1–10 10 km/s <V <V(H2)> )> ~10–100 100 km/s <V <V(Ha)> )> >30 – 500 500 km/s

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SLIDE 7

HH 212 Source NORTH 1 pc

HH 91/92 Source NORTH 1 pc

HH HH 212 (Orion

  • n B) 4.

4.5 5 µm m (H2), , 8 8 µm m HH HH 91/9 /92 (Orion

  • n B) 4.

4.5 5 µm m (H2), , 8 8 µm m (note e du dust st sh shel ell !)

Pa Parsec-sca scale e flows s from Class ss 0 YSOs

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HH 4 HH 46/47 NT NTT

[OII II] Ha Ha [SII II] = 0.38, 0.65, 0.67 µm

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HH 4 HH 46/47 S Spitzer H2 PAH PAH 3. 3.6, , 4. 4.5, , 8 µm (N (Noriega-Cr Cres espo+ + 04) 04)

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HH HH 46/4 /47 CO CO CO CO (A (ALMA), , [S [SII] ] (H (HST) T) (Ar Arce ce+ + 2013) 2013)

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HH HH 46/4 /47 (H (Hartigan et al. 05, AJ) HST HST 1994 VPM

PM ~

~ 300 300 km/s

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HST HST 1997 HH HH 46/4 /47 (Ha Hartigan et et al. 05, AJ AJ) VPM

PM ~

~ 300 300 km/s

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HH HH 46/4 /47 Ha CO CO c conf nfine ned to to <10% <10% o

  • f S

Size & & V Velocity ty ! !

(S (Stan anke, , McCau augrean an, , & Zinnecker 1999)

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Or Orion ion A

CO CO 1 1-0 0 Tpe

peak

CA CARMAOrion

(K (Kong S.

  • S. et al.

. 2018)

[SII] CT CTIO 4m 4m

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SLIDE 15

Or Orio ion OM n OMC1:

N-bo body dynam amic ics in in dense gas gas => => Orbit Orbit decay ay => => N-bo body dynam amic ics: : im importan rtant t for r IMF CO CO 1 1-0

V = V = 4 4 – 12 12 km/s Ko Kong S.

  • S. et

t al.2 .2018

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SLIDE 16

=> => 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

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SLIDE 17

=> => 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

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SLIDE 18

=> => 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

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SLIDE 19

? CO CO 1 1-0

V = V = 4 4 – 12 12 km/s Ko Kong S.

  • S. et

t al.2 .2018

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SLIDE 20

Ho How?

CO CO 1 1-0

V = V = 4 4 – 12 12 km/s Ko Kong S.

  • S. et

t al.2 .2018

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SLIDE 21

Or Orion ion A

CO CO 1 1-0 0 Tpe

peak

CA CARMAOrion

(K (Kong S.

  • S. et al.

. 2018)

[SII] CT CTIO 4m 4m

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SLIDE 22

Ho How Common are Explosive ve Outfl flows?:

Se Seve veral `fos

  • ssil’ Galactic candidates exist

~ ~ is isotro tropic ic for r ~10 ~103 ye 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 ~150 IR-on

  • nly transients in ~20 nearby star-fo

forming ng galax galaxie ies 3. 3.6 6 & 4. 4.5 5 µm 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? Ou Outf tflo lows CO CO 1 1-0

2. 2.6 6 mm

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SLIDE 23

Ho How Common are Explosive ve Outfl flows?:

Se Seve veral `fos

  • ssil’ Galactic candidates exist

~ ~ is isotro tropic ic for r ~10 ~103 ye 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 ~150 IR-on

  • nly transients in ~20 nearby star-fo

forming ng galax galaxie ies 3. 3.6 6 & 4. 4.5 5 µm 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? Ou Outf tflo lows [S [SII]

6716/ 6716/6731 6731 A

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SLIDE 24

HH HH 34 / 201 / 222 Ha Ha [S [S II

II]

]

(Re Reipurth+ Su Subaru)

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HH HH 34 / 201 / 222 Ha Ha [S [S II

II]

]

(Re Reipurth+ Su Subaru)

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Ha, , [S [SII]

Wa Walawender, Bally, y, Re Reipurth (06)

Sp Spitz tzer/IRA RAC

Jo Jorgensen et. (06)

Outflows

~150 YSOs in NGC 1333

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SLIDE 27

NGC 1333 Ha, [SII] H2

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SLIDE 28

0.15 pc

NGC 1333 8 µm CO CO

CARMA Plunkett+ (2013)

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SLIDE 29

G28.37+0.07 8 µm CO CO

ALMA Kong+ (2019)

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SLIDE 30

10-1 100 101 102 103 104 105 Source Luminosity (LO

  • )

10-7 10-6 10-5 10-4 10-3 10-2 10-1 Mechanical Force (MO

  • km s-1 yr-1)

Low-Mass High-Mass

Maud et al. (2015) Class I Class 0

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SLIDE 31
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5 7 9 km/s CARMAOrion

12CO (Kong+ 2018)

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6 8 10 km/s CARMAOrion

12CO (Kong+ 2018)

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7 9 11 km/s CARMAOrion

12CO (Kong+ 2018)

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8 10 12 km/s CARMAOrion

12CO (Kong+ 2018)

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SLIDE 36
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SLIDE 37

Ho How Common are Explosive ve Outfl flows?:

Se Seve veral `fos

  • ssil’ Galactic candidates exist

~ ~ is isotro tropic ic for r ~10 ~103 ye 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 ~150 IR-on

  • nly transients in ~20 nearby star-fo

forming ng galax galaxie ies 3. 3.6 6 & 4. 4.5 5 µm 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?

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SLIDE 38

Ho How Common are Explosive ve Outfl flows?:

Se Seve veral `fos

  • ssil’ Galactic candidates exist

~ ~ is isotro tropic ic for r ~10 ~103 ye 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 ~150 IR-on

  • nly transients in ~20 nearby star-fo

forming ng galax galaxie ies 3. 3.6 6 & 4. 4.5 5 µm 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?

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Pr Pre-ex expl plosion ca cavities es by by pre re-ex existing

  • ut

utfl flows?

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SLIDE 40
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SLIDE 41
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SLIDE 42
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SLIDE 43
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SLIDE 44
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The The O Orion E n Explosion

Nea Near-in infrared (2 µm) m) Ge Gemini-S GS GSAOI + + GE GEMS (B (Bally y et al. 2015) )

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SLIDE 46
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SLIDE 47

1999 1999

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SLIDE 48

2013 2013

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SLIDE 49

Lo Lons nsdale “ “sour urce x x” V V = 55 km/ m/s (Luhma man et et al. 2017) 1999 1999 Suba baru ru 2. 2.12 12 µm m H2 Ka Kaifu et al. 2000 BN BN n

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Lo Lons nsdale “ “sour urce x x” V V = 55 km/ m/s (Luhma man et et al. 2017) 2013 2013 Gemin ini i S 2. 2.12 12 µm m H2 Bally Bally et t al.

  • al. 2015

2015 BN BN n

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SLIDE 51

Source I BN n IRc 4 Source x

2013 2013 Ge Gemini S H2 at at 0.0 .002 mm

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x I n BN

  • 100 to 0 km/s

+20 to +120 km/s

LSR

  • Max. Temperature

V =

2015 2015 ALMA CO CO at t 1.3 mm mm (B (Bally+ y+ 2017)

~ ~15

15 Mo Sr Src I VPM

P M =

= 13 13 km/s

/ s

~3 ~3 Mo Sr Src X VPM

P M =

= 55 55 km/s

~ ~

1 1 M Mo B N B N V VPM

PM =

= 2 6 2 6 k k m m / / s s

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SLIDE 53

V =+120 km / s V = -120 km/s

North-South Cut No No de deceleration i n in w n wakes ! ! n ~ n ~ 1 100 l line near eject ejecta st stream ams s with V V pr propo portiona nal t to R

r >>

>> ram

ambient

r >

> 10 108 cm cm-3

3

N ~ N ~103 cl clumps with Mcl

clump~10

~1028

28 - 10

1030

30 gr

grams ?

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SLIDE 54
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SLIDE 55

B-fi fields? SOFIA/HAWC+ C+ Chus Chuss+2019 +2019

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SLIDE 56

Or Orio ion n OM OMC1:

Orbit Orbit deca decay No Non-hi hierarchi hical syst system Fo Form rm ~1 AU bin binary ary or

  • r mer

merger er (Sr Src I) I)? ~550 550 years rs ago ago ~10 1048

48 er

ergs Ex Expl plosion in in gas gas: : ~10 10 Mo Vma

max~400

400 km/s Eje ject t 3 3 sta tars rs: BN BN (~10 ~10 Mo) ) Sr Src I I (~15 Mo) ) Sr Src x x (~ (~3 Mo) 30 30 km km/s /s 10 10 km km/s /s 55 km km/s /s

(C (CB or merger remnan ant?)

=> => Lum umino nous us IR IR-tra transie ient t (1475+/ 1475+/-25 25 AD)

(1 (175 AD = 1475 – 1300 1300 l. l.y)

=> => N-bo body dy dynami mics cs => IMF ? (Mi

Mikko kkola & & Re Reipruth th 2015) 2015)

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SLIDE 57

Ho How Common are Explosive ve Outfl flows? ?

is isotro tropic ic for r ~10 ~103 yr yrs bip bipolar lar for r ~10 ~105 yr yrs …. …. Few w % % of

  • f ou
  • utflow
  • ws

Lum Lumino inous us E Extra-Ga Galactic IR-tr transients ts with th JWS JWST

~ ~ 3. 3.6 6 & & 4.5 µm m Spi pitzer er SPIRITS Sources ces (Ka Kaslilwal+ + 2017) 2017) No Novae, , stellar llar merge rgers rs, , SNe, , su supernova imp mpost stors Pr Protostellar mer merger ers? s?

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DR DR 21 H2 D D ~ 1.3 kpc pc

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DR DR 21 H2 D D ~ 1.3 kpc pc

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DR DR 21 H2 D D ~ 1.3 kpc pc

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DR DR 21 H2 D D ~ 1.3 kpc pc

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SLIDE 62

G34.26+0.16 C N

  • r

t h 1.08 pc 1 arc min

G3 G34.26+0.15 Sp Spitzer D D ~ 5.5 kpc pc

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SLIDE 63

Su Summary

Ou Outflo lows: Di Direct ect Feed eedback ck impact ct JW JWST: 0. 0.05” 05” [FeII] II], H2 th throu

  • ughou
  • ut

t Ga Galaxy H-re recombination lines MI MIRI spectra of mi mid-IR IR lines bands Im Imaging dust: entra rained dust, shells, & cavities Pr Protostellar E Expl plosions ns a and R nd Runa unaway s stars: N-bo body ejectio ions JW JWST: Pr Prope per m motions ns Lum Lumino nous us IR IR tra ransients

Fe Feedb dbac ack + N-bo body int interactio ions ns =>

=> IMF MF

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SLIDE 64