Lecture 10: Chemical Evolution of Galaxies
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Transcript of Lecture 10: Chemical Evolution of Galaxies
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Lecture 10: Chemical Evolution of GalaxiesMetalicity evolution Z( t ) ( vs galaxy type )
Processes that alter the metalicity:
1. Type-II SNe enrich the ISM.
2. Low-mass stars form from enriched ISM and “lock-up” metals.
3. Primordial gas falls in from IGM.
4. ISM ejected into IGM. (e.g. SN explosions, galaxy collisions)
Closed Box model: 1 and 2 only. Accreting Box: 1,2,3. Leaky Box: 1,2,4.
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M0 = total mass
MG( t ) = mass of gas in ISM
MZ ( t ) = mass of metals in ISM
M* ( t ) = mass locked up in stars and remnants
Mass conservation:
We also know:
To derive:
We will find:
Metalicity Evolution: Z(t)
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ISM Recycling Model
Yield: y = mass of metals returned to ISM per mass turned into low-mass stars and remnants
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ISM Recycling Model
From Salpeter IMF and SN1987A:
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The “Yield”
From Salpeter IMF and SN1987A:
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Differentiate:
Metalicity Evolution Z( t )
Definition of yield:
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Closed Box with constant YieldIntegrate (with y = constant ) :
At Z = 0, MG = M0 :
Note that as => 0, Z => ∞
Impossible ! :-(
What went wrong? Yield is not quite constant.
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Closed Box with varying Yield
Yield is approx constant: (1-) / ~ 0.075, (0.1)0.075=0.98 But y => 0 and Z => ZSN as = > 0 ( from
the last SN ).
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Metalicity distribution of the StarsMetalicity of stars =
Metalicity of gas from which they
formed.
“G dwarf problem”: very few sun-like stars (spectral type G) have metalicity below ½ solar.Closed Box Model FAILS: predicts that > ¼ of stars with Z < Zhave Z < ½ Z
Why are there so few low-metalicity stars?What caused the rapid initial enrichment?
Z
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What caused the initial enrichment?IGM somehow enriched before galaxies form?First generation (Pop III) Z = 0 stars all high mass?Accreting Box model with low initial gas mass and Z=>y ?
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Accreting Box varying Yield
Assume star formation proportional to gas mass
( e.g. Elliptical galaxy)
Accrete Z = 0 gas, constant dMIN / dt , until t = 100.
Closed box for t > 100.
Result: Z( t ) rises until Z ~ y( Z( t ) )
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Accreting Box, constant gas mass
Approx: Z = -y ln()
until Z = y.
dMOUT = 0dMIN = dM* => MG= constantdZ = dMZ / MG = ( y – Z ) dM*
Z stops increasing when Z => y
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Insert ( t ) for each galaxy type into
Ellipticals:
Spirals:
Irregulars:
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Ellipticals:Spirals:
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Irregulars:
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First generation: Z = 0 later generations Z << ZSN :
From Salpeter IMF and SN 1987A: = 0.93
From SN 1987A: ZSN = 0.13
Solar metals :
Milky Way has used
about 90% of its gas:
.
Initial and Effective Yield
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Effective Yield vs Galaxy MassTully-Fisher : ( M / 1011M ) ~ ( Vrot / 200 km/s )4
Lower yield in small galaxies because SN ejecta excape.
Garnett 2002
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Summary• Simple models for Z( ( t ) )
(Closed Box, Accreting Box, Leaky Box) • Yield: y = mass of metals returned to ISM per mass
turned into low-mass stars and remnantsZ = - y ln( ) = y ln( 1 / )
• “G dwarf problem” Closed Box model fails, predicts too many low-Z stars.
• Infall of Z = 0 material causes Z => y.• yeff = Zobs / ln(1/) ~ 0.01• 0.001 for small Galaxies (SN ejecta escape)
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