1. How do massive stars form? A comparison of model tracks with Herschel data Michael D Smith CAPS University of Kent Available at: http://astro.kent.ac.uk/mds/capsule.pdfhttp://astro.kent.ac.uk/mds/capsule.pdf October 2013

2. Late stage: Rosette in optical AFGL 2591 Rosette Nebula, Travis Rector, KPNO

3. Early emerging: near-infrared, with outflows Li et al 2008 ApJL 679, L101

4. K3-50 A IRAS 23151+5912 AFGL 2591 Mon R2 R Mon S140 IRS 1 S140 IRS 3 Near-Infrared Interferometry: Preibisch, Weigelt et al.

5. Numerical telescope: K-band imaging reflected shock total AFGL 2591

6. ●6●6 Approach 1: HMCs to UCHii to Hii ● Adapted from Gorti & Hollenbach 2002

7. ●7●7 Approach 2: IRDCs, ALMA, to Herschel cool cores IRDCs: initial states imprinted - SDC335 Accelerated accretion a) Mid-infrared Spitzer composite image (red: 8 μm; green: 4.5 μm; blue: 3.6 μm) b) ALMA-only image of the N 2 H + (1−0) integrated intensity, c) ALMA N 2 H + (1−0) velocity field Peretto et al 2013, 555, A112

8. ●8●8 Approach 3: two stage stitch-up Molinari et al 2008 noted: lack of diagnostic tools. Stage 1: Accretion phase Stage 2: Clean up, cluster forms + sweep out Early protostar: Accelerated accretion model (Mckee & Tan 2003) Clump mass and final star mass simply related): Accelerated accretion

9. ●9●9 Approach 3: two stage stitch-up Molinari et al 2008 tracks from SED to mm dust masses Diagnostic tools: Accelerated accretion L bol -M clump -T bol M clump /M solar

10. ● 10 Alternative evolutions Dark cloud fragments into cores/envelopes. Envelope accretion: from fixed bound envelope, bursts etc Global collapse. Accretion evolutions: from clumps, competitive, turbulent. Cores and protostars grow simultaneously Mergers, harrassment, cannabolism, disintegration

11. ● 11 Issues for Massive Stars Global collapse or fragmentation? Most massive? Radiation feedback problem + solutions Environment? Cluster-star evolutions? Which forms first? Efficiency problem. IMF: Feedback - radiation and outflow phases? EUV problem Separate accretion luminosity from Interior luminosity? Bursts? Luminosity problem: under-luminous? Two phases; accretion followed by clean-up? Dual evolution?

12. ● 12 Krumholz et al. 2007, 2009 ; Peters et al. 2010a, 2011 ; Kuiper et al. 2010a, 2011, 2012 ; Cunningham et al. 2011 ; Dale & Bonnell 2011 Kuiper & Yorke 2013: 2D RHD, core only: spherical solid-body rotation + protostellar structure. Conclusion: diverse, depends on disk formation, bloating and feedback coordination. Recent Simulations

13. ● 13 Objective: Model for Massive Stars Piece together evolutionary algorithms for the protostellar structure, the environment, the inflow and the radiation feedback. The framework requires the accretion rate from the clump to be specified. We investigate constant, decelerating and accelerating accretion rate scenarios. We consider both hot and cold accretion, identified with spherical free-fall and disk accretion, respectively.

14. ● 14 Objective: Model for Massive Stars Piece together evolutionary algorithms for the protostellar structure, the environment, the inflow and the radiation feedback. The framework requires the accretion rate from the clump to be specified. We investigate constant, decelerating and accelerating accretion rate scenarios. We consider both hot and cold accretion, identified with spherical free-fall and disk accretion, respectively.

15. ● 15 Cold or Hot Accretion? Kuiper & Yorke 2013 ApJ 772 Hosokawa, Omukai, Yorke 2009, 2010

16. ● 16 The protostar: radius Stellar radius as mass accumulates (I) adiabatic, (II) swelling/bloating, (III) Kelvin–Helmholtz contraction, and (IV) main sequence Hot accretion Cold accretion

17. ● 17 The protostar: luminosity Origin Luminosity as mass accumulates (cold)

18. ● 18 The protostar: adaption Assumed mass accretion rates + interpolation scheme

19. ● mass conservation ● prescribed accretion rate ● bifurcation coefficient ● jet speed ~ escape speed The Low-Mass Scheme: Construction ● Clump Envelope Accretion Disk Protostars ● Bipolar Outflow Jets ● Evolution: ● systematic and simultaneous Protostar L(Bolometric) Jet L(Shock) Outflow Momentum (Thrust) Clump/Envelope Mass Class Temperature Disk Infrared excess

20. The Capsule Scheme: Construction ● Clump Envelope Accretion Disc Protostar Bipolar Outflow Jets Lyman Flux thermal radio jets H 2 shocks Radiative Flux Radio: H II region

21. ● 21 Capsule Flow Chart

22. Origin Luminosity as clump mass declines ● 22 The clump mass, isotherms + Herschel data Accelerated accretion Power Law deceleration (Data: Molinari et al 2008) Constant slow accretion Accelerated accretion ( Data: Elia et al 2010), Hi-GAL

23. Origin Distance dotted line = accelerated accretion ● 23 Bolometric Temperature Herschel: <20K: 0.463 <30K: 0.832 <50K: 0.950

24. ● 24 Bolometric Temperature Clump = cluster x 6 Clump = cluster x 2

25. ● 25 L bol -M clump -T bol results Accelerated accretion is not favoured Source counts as a function of the bolometric temperature can distinguish the accretion mode. Accelerated accretion yields a relatively high number of low-temperature objects. On this basis, we demonstrate that evolutionary tracks to fit Herschel Space Telescope data require the generated stars to be three to four times less massive than in previous interpretations. This is consistent with star formation efficiencies of 10-20%

26. Or Luminosity as clump mass declines: massive clumps ● 26 The clump mass, isotherms + Herschel data

27. ● 27 The Lyman Flux (ATCA 18 GHz data) Orig Accelerated accretion L bol /L sun Bolometric Luminosity Sanchez-Monge et al., 2013, A&A 550, A21

28. Origin D COLD accretion + Hot Spots (75%, 5% area) Distributed accretion Accretion hotspots ● 28 The Lyman Flux Orig Constant accretion rate

29. Neither spherical nor disk accretion can explain the high radio luminosities of many protostars. Nevertheless, we discover a solution in which the extreme ultraviolet flux needed to explain the radio emission is produced if the accretion flow is via free-fall on to hot spots covering less than 20% of the surface area. Moreover, the protostar must be compact, and so has formed through cold accretion. This suggest that massive stars form via gas accretion through disks which, in the phase before the star bloats, download their mass via magnetic flux tubes on to the protostar. ● 29 The Lyman Flux: summary

30. Or Different constant accretion rates……….. ● 30 Jet speed = keplerian speed

31. ● Michael D. Smith - Accretion Discs ● 31 What next? ● Disk – planet formation ● Binary formation, mass transfer etc ● Mass outflows v. radiation feedback ● Feedback routes ● Outbursts ● Thermal radio jets ● ???

32. Thanks For Listening! ANY QUESTIONS?

33. ● X-Axis: Luminosity ● Y-Axis: Jet Power ● Tracks/Arrows: the scheme ● Diagonal line: ● Class 0/I border ● Data: ISO FIR + NIR (Stanke) ● Above: Class 0 ● Under: Class 1 Low-Mass Protostellar Tracks

34. ● Michael D. Smith - Accretion Discs ● 34 Disk evolution ● Column density as function of radius and time: (r,t) ● Assume accretion rate from envelope ● Assume entire star (+ jets) is supplied through disc ● Angular momentum transport: ● - turbulent viscosity: `alpha’ prescription ● - tidal torques: Toomre Q parameterisation ● Class 0 stage: very abrupt evolution?? Test…… ● …to create a One Solar Mass star

35. ● Michael D. Smith - Accretion Discs ● 35 The envelope-disc connection; slow inflow ● Peak accretion at 100,000 yr ● Acc rate 3.5 x 10 -6 Msun/yr ● Viscosity alpha = 0.1 ● 50,000 yr: blue ● 500,000 yr: green ● 2,000,000 yr: red

36. ● Michael D. Smith - Accretion Discs ● 36 The envelope-disc connection; slow inflow; low alpha ● Peak accretion at 200,000 yr ● Acc rate 3.5 x 10 -6 Msun/yr ● Viscosity alpha = 0.01 ● 50,000 yr: blue ● 500,000 yr: green ● 2,000,000 yr: red