16.05.07 Markus Wadepuhl Stellar evolution and Stellar evolution and nucleosynthesis nucleosynthesis
16.05.07 Markus Wadepuhl
Stellar evolution and Stellar evolution and
nucleosynthesisnucleosynthesis
16.05.07 Markus Wadepuhl
OutlineOutline� The sun: models and nuclear reactions
– pp-chain
– CNO-cycle
� Steps in nucleosynthesis
– He-burning
– C-burning
– O-burning
� Uncertainties
� The share of stellar nucleosynthesis in galactical abundance
16.05.07 Markus Wadepuhl
The stellar modelThe stellar model� Needs to follow the basic equations of
stellar evolution
ρπ 24
1
rm
r=
∂
∂2
2
244
1
4 t
r
rr
Gm
m
P
∂
∂−−=
∂
∂
ππ t
P
t
Tc
m
lpn
∂
∂+
∂
∂−−=
∂
∂
ρ
δεε υ
∇−=∂
∂
Pr
GmT
m
T44π
−=
∂
∂∑∑
k
ik
j
jiii rr
m
t
X
ρ
� Inserting the known values for the sun yields
16.05.07 Markus Wadepuhl
The solar modelThe solar model
16.05.07 Markus Wadepuhl
The The pppp--chain (Tchain (T66 < 15)< 15)
� first step very unusual due to the β+ decay at
the time of the closest approach
� pp II and pp III gain in importance with
increasing temperature
16.05.07 Markus Wadepuhl
The CNOThe CNO--cycle (Tcycle (T66 < 50)< 50)
� C, N and O act similar to catalysts
� Maincycle dominates (≈ 1000 times)
�14N acts as a „bottleneck“
– Nearly all initially present C, N and O nuclei
will be found as 14N
16.05.07 Markus Wadepuhl
The CNOThe CNO--cyclecycle
� With increasing
temperature the CNO-
cycle gains in
importance
� Other situation for
population III stars
(no CNO cycle)
16.05.07 Markus Wadepuhl
Solar NeutrinosSolar Neutrinos
� pp-chain as well as the CNO-cycle produce
a characteristic neutrino spectrum
� neutrinos can easily escape and carry away
their energy
� good test for solar models
16.05.07 Markus Wadepuhl
Steps in nucleosynthesisSteps in nucleosynthesis
� after Hydrogen is exhausted, there are
several burning stages that can be ignited at
higher and higher temperatures
(depending on the initial mass and
composition of the star)
� different burning stages can occur parallel
in different regions of the star
(shell burning, onion skin structure)
16.05.07 Markus Wadepuhl
Steps in nucleosynthesisSteps in nucleosynthesis� during carbon burning and the later stages
many neutrinos are produced
– high energy loss by neutrino emission
Woosley et. al., 2002, RvMP, 74, 1016
16.05.07 Markus Wadepuhl
Helium Burning (THelium Burning (T88 > 1)> 1)
BeHeHe844 ⇔+ � Decays after ≈ 10-16 s
γ+→+ CHeBe 1248
γ+→+ OHeC 16412
γ+→+ NeHeO 20416
� Following processes possible but in typical
stellar-environment very rare
( ) ( ) ( ) ( ) MgnNeOeFN 2522181814 ,,, αγαυγα +
� Produces free n that can form heavy
Elements (A ≥ 60)
16.05.07 Markus Wadepuhl
Carbon Burning (TCarbon Burning (T88 = 5..10)= 5..10)
pNaCC +→+ 231212
α+→+ NeCC 201212
( ) NepNa 2023 ,α
� p and α find themselfes at extremely high
temperatures (too high for H and He burning)
� New reactions with other particles in the mixture
( ) ( ) ( ) OnCeNpC 16131312 ,, αυγ +
16.05.07 Markus Wadepuhl
PhotodisintegrationPhotodisintegration
(Neon Burning)(Neon Burning)� For T9 > 1 photodisintegration occurs
( ) ONe 1620 ,αγ
� Several following reactions are possible
γγ ++→+ MgONe 2416202
( ) ( ) ( ) SiMgNeO 28242016 ,,, γαγαγα
( ) SinMg 2825 ,α ( ) SinMg 2926 ,α ( ) AlnpMg 2626 ,
( ) SiMg 3026 ,γα ( ) SipAl 3027 ,α ( ) PpSi 3130 ,γ
� Main energy production via
( ) AlpMg 2625 ,γ
16.05.07 Markus Wadepuhl
Oxygen Burning (TOxygen Burning (T99 > 1)> 1)
pPOO +→+ 311616 α+→+ SiOO 281616
� same problem with p and α as during the carbon
burning
� Produces many nuclei e. g.28Si, 32,33,34S, 35,37Cl, 36,38Ar, 39,41K, 40,42Ca
16.05.07 Markus Wadepuhl
PhotodisintegrationPhotodisintegration
(Silicon Burning)(Silicon Burning)
� at even higher temperatures (T9 > 3) 28Si can also
be decomposed
� n, p and α react with 28Si and build gradually
heavier nuclei until 56Fe is reached
( ) ( ) ( ) ( ) ( )ααγαγαγαγαγ 2,,,,, 1216202428 CONeMgSi
( ) ( ) ( ) ( ) ( ) SinSinSipPpSSi 282930313228 ,,,,, γγγγγα
16.05.07 Markus Wadepuhl
Chronological DevelopmentChronological Development
Woosley et. al., 2002, RvMP, 74, 1016
16.05.07 Markus Wadepuhl
Chronological DevelopmentChronological Development
Woosley et. al., 2002, RvMP, 74, 1016
16.05.07 Markus Wadepuhl
Chronological DevelopmentChronological Development
� onion skin structure
16.05.07 Markus Wadepuhl
UncertaintiesUncertainties
� Convection
– Diffusion coefficient is modeled with a typical
mixing length
– Nuclear burning is carried out first
– Afterwards mixing is applied
� Nuclear reaction rates( ) OC 1612 ,γα ( ) MgnNe 2522 ,α
16.05.07 Markus Wadepuhl
ConvectionConvection
Woosley et. al., 2002, RvMP, 74, 1016
16.05.07 Markus Wadepuhl
ConvectionConvection
Woosley et. al., 2002, RvMP, 74, 1016
16.05.07 Markus Wadepuhl
ConvectionConvection
Woosley et. al., 2002, RvMP, 74, 1016
16.05.07 Markus Wadepuhl
ConvectionConvection
Woosley et. al., 2002, RvMP, 74, 1016
16.05.07 Markus Wadepuhl
UncertaintiesUncertainties� rotation
– centrifugal effects
– transfer of angular momentum may cause wind
� magnetic fields
– cause magnetic torques between differencially
rotating shells
� binaries
– Mass transfer between the two components if Roche
lobe is crossed
� winds
– depends crucially on the inital mass and metallicity
16.05.07 Markus Wadepuhl
Mass lossMass loss
Woosley et. al., 2002, RvMP, 74, 1016
16.05.07 Markus Wadepuhl
Mass lossMass loss
Woosley et. al., 2002, RvMP, 74, 1016
16.05.07 Markus Wadepuhl
The influence of metallicityThe influence of metallicity
Heger et al., 2003, APJ, 591, 288
16.05.07 Markus Wadepuhl
Chemical compositionChemical composition
Woosley et. al., 2002, RvMP, 74, 1016
16.05.07 Markus Wadepuhl
Chemical compositionChemical composition
Woosley et. al., 2002, RvMP, 74, 1016
16.05.07 Markus Wadepuhl
The ISM yield The ISM yield
� Winds
– Not well understood
� SNe
– mass cut
– explosion mechanism
– consider fallback
– very complicated explosive processes
� Plot the production factor
– Xi / Xi sol
16.05.07 Markus Wadepuhl
Chemical compositionChemical composition
Woosley et. al., 2002, RvMP, 74, 1016
16.05.07 Markus Wadepuhl
Special issuesSpecial issues
� especially metal-poor population III stars
possibly were very massiv
– maybe different SNe mechanism
� unknown mass cut
� rather simple explosion modeling
– Piston model
� only very few detailed SN observations
16.05.07 Markus Wadepuhl
ReferencesReferences
� A. Unsöld & B. Baschek. Der neue Kosmos. Springer, Berlin, 2005
� R. Kippenhahn & A. Weigert, Stellar Structur and Evolution, Springer, Berlin, 1990
� D. Arnett, Supernovae and Nucleosynthesis, Princeton University Press, Princeton, 1996
� G. Wallerstein et al. Synthesis of the elements in stars: forty years of progress. RvMP 69: 995 – 1084, 1997
� S. E. Woosley et al. The evolution and explosion of massive stars. RvMP 74: 1015 – 1064, 2002
� A. Heger et al. The nucleosynthetic signature of population III. ApJ 567: 532 – 543, 2002
� K. Nomoto et al. Hypernovae and their Nucleosynthesis. Astro-ph/0209064
� A. Heger et al. How massive single stars end their life. ApJ 591: 288 – 300, 2003
� T. Rauscher et al. Nucleosynthesis in massive stars with improved nuclear and stellar physics. Astro-ph/0112478v2