Alessandro Chieffi - Landessternwarte Heidelberg-KönigstuhlAlessandro Chieffi Istituto Nazionale di...
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11th Symposium on Nuclei in the Cosmos (NIC XI) Heidelberg, 19-23 July 2010 Alessandro Chieffi Istituto Nazionale di AstroFisica (Istituto di Astrofisica Spaziale e Fisica Cosmica) & Centre for Stellar and Planetary Astrophysics – Monash University - Australia Email: [email protected] Marco Limongi Istituto Nazionale di AstroFisica (Osservatorio Astronomico di Roma) & Centre for Stellar and Planetary Astrophysics – Monash University - Australia Email: [email protected] The final stages of stellar evolution
Transcript of Alessandro Chieffi - Landessternwarte Heidelberg-KönigstuhlAlessandro Chieffi Istituto Nazionale di...
11th Symposium on Nuclei in the Cosmos (NIC XI)
Heidelberg, 19-23 July 2010
Alessandro ChieffiIstituto Nazionale di AstroFisica (Istituto di Astrofisica Spaziale e Fisica Cosmica)
&
Centre for Stellar and Planetary Astrophysics – Monash University - Australia
Email: [email protected]
Marco LimongiIstituto Nazionale di AstroFisica (Osservatorio Astronomico di Roma)
&
Centre for Stellar and Planetary Astrophysics – Monash University - Australia
Email: [email protected]
The final stages of stellar evolution
H
He
CO
Fe
ZrBa
Th
Zn
Pb
N
Li
Be
B
F
NeSi
S
Ca
Ti
Ar Ni
Kr
Mo Sn
Nd
Yb
Solar chemical composition
Slide stolen from Nikos Prantzos
120 MO
12 MO
Si
H
He
C
NeO
Convective zones
RSG RSG+WR BSG+WR
WNE
WNL
WCO
BLACK HOLE
NEUTRON STAR
Type II
Type I bc
Final mass
RSG RSG+WR BSG+WR
WNE
WNL
WCO
BLA
CK
H
OLE
NEUTRON STAR
Type II
Type I bc
Final mass
NEUTRON STAR
Initia
l m
ass
Base
con
vect
ive
enve
lope
H c
onve
ctiv
e co
re
M
HC=0
He
core
He convecti
ve
core
He convective shell
C convective shellOuter border of the explosive burningsFe core
mass
CO core
Mass Loss in the WNE / WCO phases: Langer89 - Nugis & Lamers 001 foe
Mass Loss in the WNE / WCO phases: Langer89 - Nugis & Lamers 001 foe
Which is the role of the advanced burning phases in the yield production?
shape the final mass – radius relation
model the final Ye profile
determine the size of the “Fe” core
influence the explosive yields
Through the extension of the Si convective shell
Determine the C&Ne abundances in the C convective shell
Determine the final abundances of the nuclei produced by the quiescent C burning: i.e. Ne, Na, Mg, Al + weak S process nucleosynthesis
FRANEC 6.0
Major improvements compared to the release 4.0 (Limongi & Chieffi 2003, Chieffi & Limongi 2004) and 5.0 (Limongi & Chieffi 2006)
- FULL COUPLING of: Physical Structure - Nuclear Burning - + Chemical Mixing (convection, semiconvection, rotation)
- INCLUSION OF ROTATION: Transport of Angular Momentum (Advection/Diffusion)
- MASS LOSS (Enhanced mass loss for RSG phase, Van Loon 2005)
- SOLAR COMPOSITION (Asplund et al. 2009)
- TWO NUCLEAR NETWORKS: 163 isotopes (448 reactions) H/He Burning 282 isotopes (2928 reactions) Advanced Burning
FRANEC 6: current release 6.100503
f P=4r
4
G M Sg eff−1
dPdM
=−G M
4r4⋅ f P
dMdr
=4r2
d lnT
d lnP
=3 L P
16 acGT 4 M
⋅f Tf p
f T=162 r
4
S2g eff
−1g eff
dL=M
d Y id t
= ∂Y i∂ t nuc ∂∂m [ 4 r2
2D semiDmixDrot
∂ x i∂m ] i=1. ..N
1 systemof M meshes⋅N isotopes5ODEs
ddt
r 2M r=1
r 2∂∂ r [r 4D shear
130r∣U∣
∂
∂ r ]or
ddt
r 2M r=0
ddt
r 2M r=151
r 2∂∂ r
r 4U 1r 2
∂∂ r r4D shear
∂
∂ r 4 ODEsU( Maeder & Zahn 1998)
U(Kippenhahn & Weigert 1990)
25 MO - Z=ZO
mass
He convective shell
C convective shellsHe c.c.
H c.c.
Log10
(tfinal
-t)
O Si
25 MO - Z=ZO
mass
He convective shell
O convective shell
Initial equatorial velocity 300 Km/s
Log10
(tfinal
-t)
H c.c.
He c.c. CO Si
Ye
C
O
Ne
Si
25 MO - Z=ZO O.50
O.45
He
Ye
C
O
Ne
Si
25 MO - Z=ZO O.50
O.45
He
25 MO - Z=ZO SiXC SiXSiXCSiXCSiXC OX NeX and CX
Ye
C
O
Ne
Si
M
O.50
O.45
