the feeding and feedback of massive protostars
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The feeding and feedback of massive protostars. Michael D Smith et al. CAPS University of Kent September 2012. Talk outline. The Model: Scenarios, Mechanisms and Stages Scheme construction Feeding: clump to envelope to disc to star+jets - PowerPoint PPT PresentationTRANSCRIPT
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The feeding and feedback of massive protostars
Michael D Smith et al. CAPS
University of Kent
September 2012
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Talk outlineThe 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
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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
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● Michael D. Smith - Accretion Discs
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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
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Red X Radio sources (VLA)
Blue <> millimetre cores
Yellow + sub-millimetre cores
Green Optical HH shocks
Light blue Infrared sources
Contours H2 moleculesImage H(alpha) / S[II]
● The Confusion
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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?
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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?
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● mass conservation● prescribed accretion rate● bifurcation coefficient● jet speed ~ escape speed
The Unification Scheme: Construction● Clump Envelope Accretion Disc 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
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The Unification Scheme: Construction
● Clump Envelope Accretion Disc Protostar
● Bipolar Outflow Jets
● Lyman Flux
● thermal radio jets
● H2 shocks
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The protostar
rigin ofStellar radius as mass accumulates: hot
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The protostar
rigin ofStellar radius as mass accumulates: cold
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The protostarOrigin Luminosity as mass accumulates
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Origin Luminosity as clump mass declines
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The clump mass
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Origin Luminosity as clump mass declines
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The clump mass
Orig Accelerated accretion Power Law deceleration
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Origin Herschel cores + model temperture
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The clump mass
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Origin Distance
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The Jet Speed: hot
Orig
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Origin Distance
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The Jet Speed: cold
Orig
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Origin Distance Distance-immune evolution
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The Lyman Flux
Orig Accelerated accretion
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Origin Distance Distance-immune evolution
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The Lyman Flux
Orig Power Law deceleration
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20% Discount Code F1ASTROJET
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● X-Axia: 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
Protostellar Tracks
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● Michael D. Smith - Accretion Discs
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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
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● Michael D. Smith - Accretion Discs
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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
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● Michael D. Smith - Accretion Discs
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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