evolution models of low metallicity stars
DESCRIPTION
EVOLUTION MODELS OF LOW METALLICITY STARS. Georges Meynet, André Maeder, Sylvia Ekström. Geneva Observatory. and Raphael Hirschi Basel University. Spite et al. 2005 Cayrel et al. 2004. Early chemical evolution of galaxies. Reionization at high redshift. Pelló et al. 2004. - PowerPoint PPT PresentationTRANSCRIPT
EVOLUTION MODELS OF LOW METALLICITY STARS
Georges Meynet, André Maeder, Sylvia Ekström
Geneva Observatory
Reionization at high redshift
Spite et al. 2005Cayrel et al. 2004
Early chemical evolution of galaxies
Stellar population in metal poor and/or high redshifted galaxies
Pelló et al. 2004
and Raphael HirschiBasel University
What is different at very low Z ?
• The initial masses of the stars (?)
• The ignition of H-burning in massive stars (no CNO element catalysts at the beginning)
• The opacities are lower
Stars more compact: R(popIII) = R(Zsol)/4
Stellar winds are weaker
El Eid et al 1983; Ober et al 1983; Bond et al 1984; Klapp 1984; Arnett 1996; Limongi et al. 2000; Chieffi et al. 2000; Chieffi and Limongi 2002;Siess et al. 2002; Heger and Woosley 2002; Umeda and Nomoto 2003; Nomoto et al. 2003; Picardi et al. 2004; Gil-Pons et al. 2005
GRATTON-
ÖPIK CELL
Cells of meridional circulation
Very importantprocess for thetransport of theangular momentum
Inner cell inwards transportof angular momentumOuter cell outwards transportof angular momentum
20 Msol on the ZAMS
Timescale a few times the Kelvin-Helmholtz timescale
y000 14034000
2
4
KHKEP
THE SHEAR INSTABILITY
Where does the energy come from ?
When does it occur ?
The timescale
From the excess energy in the shear
When the excess energy in the shear canovercome the stable pressure gradients
Secular shear much longer than MS lifetimeDynamical shear dynamical timescale
Brueggen & Hillebrandt 2001
ROTATION AND MASS LOSS
WHEN Z
SURFACE VELOCITY DURING THE MAIN-SEQUENCE PHASE
WHAT CHANGES AT VERY LOW Z FOR ROTATING MODELS ?
Less angular momentum removed by stellar winds
Steeper gradients of the angular velocity in the interiors
MORE EFFICIENT MIXING
BREAK-UP LIMIT
Meridional velocities smaller
MORE ANGULAR MOMENTUM IN THE CORE
Meynet and Maeder 2003
New grids of stellar models
Also Z=0.040; 0.008, 0.004, 0.00001,10-8
+Pop IIISee talk by S. Ekström
60 Msol, vini= 0 km s-1 vini= 300 km s-1
WR:post H-b.Mass loss
WR:in H-b.Rot. mixing
<V>O=189km/sMtot
Mcc
H-b. He-b.
Enter WR phase during the MS phase
Rotating model
With a much higheractual mass: 45 Msol instead of 27 Msol
WR phase longerMass loss and Mixing
Both important
cf also Maeder 1987Fliegner and Langer 1995
For a given metallicity, the minimum initial mass of single stars which become Wolf-Rayet star is decreased for higher rotation velocities
37Msol
22Msol
WR lifetimes alsoincreased for a given initial mass
Meynet and Maeder 2005
Observed points from Prantzos and Boissier (2003)
Meynet and Maeder 2005
Israelian et al. 2004Centurion et al 2003 (DLA)
Spite et al 2005
IMPORTANT AMOUNTS OF PRIMARY NITROGEN NEED TO BE PRODUCED AT LOW Z
60 Msol, Z=10-5, ini/= 0.85
ROTATION INDUCES NUMEROUS PROCESSES WHICH ENHANCES MASS LOSS
1) Reaching of the break-up limit during the Main Sequence phase
Cf also Sackman & Anand 1979; Langer 1998
Vcrit
Vcrit
Vini=500 km/s
Vini=300 km/sVini=300 km/s
Vini=800 km/s
60 Msol, Z = 0.020 60 Msol, Z = 0.00001
2) Redwardsevolutionfavoured
3) -limit at the tip of the blue loop
4) Surface enrichments
During the MS phaseN increased C and O decreasedbut CNO/Z remainsconstant equal to theinitial value
At the end of the coreHe-burning phase, apparitionat the surface of bothH and He-burning productsPrimary N Primary C Primary OCNO/Z increases
Vini/Vcrit~0.6 - 0.7Z=10-5
60 Mo
7 Mo
7 Mo stellar model more mixed than the 60 Mo
Gradient of steeperRadius smaller (~factor 5)Lifetime longer (~factor 9)
7 Mo
7 Msol, Z=10-5
E-AGB phase
60 Msol, Z=10-5,
C-burningphase
NUMEROUS INTERESTING CONSEQUENCES
• Higher surface enrichments at low Z Maeder &Meynet 2001; Venn & Przybilla 2003
• Change with Z of populations of Be stars Maeder et al. 1999
of blue to red supergiant ratio Langer & Maeder 1995; Maeder &Meynet 2001
of LBV and WR stars Fliegner & Langer 1995; Meynet & Maeder 2005
of type Ibc to II SN ratio Prantzos & Boissier 2003; Meynet & Maeder 2005
of collapsar progenitors MacFadyen & Woosley 1999; Hirschi et al 2005
• Change with Z of the stellar yields Meynet & Maeder 2002; Ekström et al. in prep.
A LOT OF INTERESTING PROBLEMS TO STUDY…
CONCLUSION
The effects of rotation are amplified at low metallicity mixing enhanced induce mass loss
A FEW EXAMPLES
Observations
• How fast are rotating low metallicity massive stars ?• Are their surface enrichment on average higher than at solar metallicity ?
Theory
• How stellar winds behave when CNO is increased at the surface during a red supergiant phase ?• How the evolution into the Pair Instability regime is changed by rotation ?• Might the first stellar generations enrich the ISM in new synthesized Helium ?• How the core collapse supernova explosions are affected by rotation ?• How the formation process of massive star is affected by rotation ?
ENERGY OF ROTATION
15 Msol
crit (ini)=~0.6
Gravitational energy
1050.3 ergs
Veq [km s-1]
Energy of reference gravitational energy
Thermal energy ~50%
Energy of radiation ~10%
Rotational energy ~0.3%
Excess of energy in the shear ~0.003%
Thermal energy
Energy of radiation
Energy of rotation
Excess energy of shear
Mass fraction of hydrogen at the center
GLOBAL MASS LOSS RATES
11
1,2
2
11
.
.
94
1
1
)0(
)(
critvvM
M
Maeder and Meynet 2000
Enhancement at break-up velocity
Log Teff 4.35 4.30 4.00 3.90
!
• The - Limit: classical Eddington limit. Non rotating LBV
• The - Limit: rotational effect dominates. Be – stars.
• The - Limit: both rotation and radiation. Most LBV.
Humphreys, 2002
0.90
0.53
0.36
What physicsmakes the Humphreys-Davidson Limit ?
LBV
WN
LBV earlierthan WN starsin general, butalso simultaneous
TRANSITION
Same mass lossfor LBV and WN9-11Crowther 1997
EVOLUTIONARYSTATUS OF LBV
A STRIKING OBSERVATIONAL FACTS
Very Helium-rich stars in Centuri ?
Y/Z
remaining mass in solar masses
60 Msol
Z = 10-8
r
XDDr
rrt
X ischeareff
i )(1 2
2
rDr
rrUr
rrt
rschear
42
42
2 1
5
1)(
Transport of the chemical speciesTransport of the angular momentum
Meridional circulation Shear turbulence
Zahn 1992
• Different evolution of the surface velocity
•When stellar winds are weak, stars can reach more easily the critical velocity
•The account for anisotropic massloss favours break-up Maeder, 2002
ROTATION AND MASS LOSS
40 Msol, Vini=400 km/s