Download - Nuclear Astrophysics (2)
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Types of Equilibria
● Steady Flow of Reactions● Chemical Equilibrium of Reactions● Complete Chemical Equilibrium (NSE)● Clusters of Chemical Equilbrium (QSE)● QSE Clusters linked by Steady Flow
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CNO(I)Cycle in Steady Flowthe network entry for nuclei with mass numbers A=12, 13, 14, 15 is governed in each case by a production reaction (proton reaction on A1) and a distruction reaction (proton reaction on A). In case of a steady flow they cancel and lead to Y=0 for all A, linking all of these terms and identical to (A=14 is useful as this encounters the slowest reaction and essentially all mass assembles in 14N)
summing all mass fractions of CNO nuclei for solar metallicity
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sprocess and steady flow
sprocessrprocesspprocess
(from Anders & Grevesse)Solar abundances (Anders & Grevesse)
shown are s, r, and ponly nuclei!
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sprocess and steady flowpossible destruction of nucleus (Z,A)
betadecay to (Z+1,A)
only one nucleus per A needs to be considered!
in case of steady flow =0
= therefore
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The sigma*Ncurve
a complete steady flow is not given, but in between magic numbers (where the neutron capture cross sections are small) almost attained!
double values due to branchings
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s and rdecomposition
the almost constant sigma*Ncurve leads to a large oddeven staggering in the abundances (due to the oddeven staggering in ncapture cross sections!
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Steady flows and chem. equilibrium in stellar burning
ppcycles and CNOcycle lead to steady flows in Hburning
4He+4He 8Be is in chemical equilibriumreleased neutrons lead to steady flow in neutron capture
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Complete chem. equilibrium (NSE)
Siburning in stellar evolution and expl. Siburning at high densities lead to NSE!
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Astrophysical Sites
main sequence
HertzsprungRussell Diagram of Stellar Evolution from Iben, showing as end stages
● white dwarfs
and
● (core collapse) supernovae
main sequience
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Type Ia Supernovae from Accretion in Binary Stellar Systems
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Back of the Envelope SN Ia
P. Höflich
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Neutronization via electron capture(high Fermi energies at central densities)
(a) Test for influence of new shell model electron capture rates (LMP)(b) Test for burning front propagation speed
56Fe
56Ni
54Fe (58Ni)
50Ti,54Cr
dominant NSEabundance
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Ignition density determines Ye and neutronrichness of (6070% of) Fegroup
results of explosive C, Ne, O and Siburning:Fegroup to alphaelements 2/13/1
SNe Ia dominate Fegroup, overabundances by more than factor 2 not permitted central density <4 109 gcm3
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Core Collapse Supernovae from Massive Stars
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QSE in low density expl. Siburningdisconnected light element (n,p,He) and SiFe QSEcluster, high alphaabundanceprefers alpharich nuclei (58Ni over 54Fe), Y
e determines dominant QSEisotope.
5
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QSE in explosive Siburning
full NSE is not attained, but there exist equilibrium groups around 28Si, 56Ni and n,p,4He, which are separated by slow reactions
Sample Calculations from ● B.S. Meyer and ● Hix and Thielemann
small Qvalues of reactions out of Z=20, N=20 cause small cross sections and hold up equilibrium
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QSE Formalismlight group
Sigroup
Ni/Fegroup
time evolution for those quantities which are in equilibrium and the individual abundances of nuclei with slow reactions which link equilibrium groups (Hix, PareteKoon, Freiburghaus, Thielemann 2007)
binding energy differences, i.e. masses enter directly
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Obtaining quilibrium at high T
at T=4 GK the equilibrium description is correct after about 103 s!
accuracy
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Incomplete Siburning with freezeout
energy generation
chargedparticle freezeout below T=3.5 GK
circles >106, squares >1012, triangles >1020
filled/open network size
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Normal and alpharich freezeout
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Interim conclusions● steady flows are approached in many hydrostatic
burning stages during stellar evolution, including the sprocess. They are determined by rates (often the smallest ones), which are/can be related to small Qvalues.
● NSE/QSE equilibria are obtained in hydrostatic Siburning and in explosive burning. Abundance distribution depends directly on mass differences, but for these applications mostly close to stability.
● How about QSEequilibria linked by steady flows (and far from stability)?