The feeding and feedback of massive protostars

1. The feeding and feedback of massive protostars Michael D Smith et al. CAPS University of Kent September 2012

2. Talk outline The Model: Scenarios, Mechanisms and Stages • Scheme construction • Feeding: clump to envelope to disc to star+jets • Evolutionary Model (abrupt, gradual, episodal, eruptive) • Feedback predictions • Global predictions

3. The Revolution • Rapid conception - turbulence ephemeral clouds • The Birth: abrupt Class 0 high accretion • Powerful jets: strong extraction • Form in clusters in giant clouds spatial distribution • Brown dwarfs and planets mass distribution • Starbursts global evolution • Primordial stars: early re-ionisation z=20 stars Turbulence, Gravity, Feedback, Regulation, Interaction, Triggering: COMPLEX SYSTEM

4. Michael D. Smith - Accretion Discs Star & Planet Building • Discs evolve: massive to light • Accretion rate determined by envelope • No single development (numerical + observed) • MSN is irrelevant: far exceeded in Class 0/I stages • Star and planets form out of the same disc Turbulence, Gravity, Feedback, Regulation, Interaction, Triggering: COMPLEX SYSTEM

5. The Confusion Red X Radio sources (VLA) Blue <> millimetre cores Yellow + sub-millimetre cores Green Optical HH shocks Light blue Infrared sources Contours H2 molecules Image H(alpha) / S[II]

6. Motivation Dedication to massive stars How? How do the observable phenomena/components correlate? Is there a systematic evolution? Tracks? Why? What processes and physics are implied?

7. Specific Motivations Where does the angular momentum end up? Are jets a necessity? Why don’t clusters overheat? When can jets occur along with HII regions? Is the accretion hot/cold/outbursting?

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

9. The Unification Scheme: Construction Lyman Flux Clump Envelope Accretion Disc Protostar Bipolar Outflow Jets thermal radio jets H2 shocks

10. The protostar rigin ofStellar radius as mass accumulates: hot

11. The protostar rigin ofStellar radius as mass accumulates: cold

12. The protostar Origin Luminosity as mass accumulates

13. The clump mass Origin Luminosity as clump mass declines

14. The clump mass Origin Luminosity as clump mass declines Orig Accelerated accretion Power Law deceleration

15. The clump mass Origin Herschel cores + model temperture

16. The Jet Speed: hot Origin Distance Orig

17. The Jet Speed: cold Origin Distance Orig

18. The Lyman Flux Origin Distance Distance-immune evolution Orig Accelerated accretion

19. The Lyman Flux Origin Distance Distance-immune evolution Orig Power Law deceleration

20. 20% Discount Code F1ASTROJET

21. Protostellar Tracks • X-Axia: Luminosity • Y-Axis: Jet Power • Tracks/Arrows: the scheme • Diagonalline: • Class 0/I border • Data: ISO FIR + NIR (Stanke) • Above: Class 0 • Under: Class 1

22. Michael D. Smith - Accretion Discs Disc 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

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

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