Download Unstable Isotopes / Explosive Burning

Unstable Isotopes / Explosive Burning
Victoria
UW
Belfast
UMinnesota
UW Madison
MIT
MSU
Stony Brook
Argonne
UCB
UCSC
ND
UOhio
Princeton
UCSB
LANL
Caltech
ASU
UTennessee
NC State
UNC Chapel Hill
Clemson
UofA
Core Institution
Senior Investigator Institution
Collaborator Institution
UAlabama
UT Austin
Monash
JINA-CEE is having a major impact over the entire stellar mass range.
papers
70
250
35
0
citations
500
2015
Through April 2016
0
2015
Through April 2016
refereed papers only.
estimated accuracy ~20%.
16
h-index
15000
8
7500
0
0
reads
odels
al M
c
i
am
yn
d
H-Burn
mo
he Chemical
A1.1
He-Burn
A1.2
C-Burn
A1.3
Supernovae
A3.5
Screening
A1.4
Weak
Reactions
A1.5
r- and
νp-process
A3.3
First
Stars
A3.1
Observations
A2.1
Neutron
Production
A1.6
ions
vat
ser
Ob
i-process
A3.2
Str
a
t
e
gic
A
re
a
ics
phys
o
r
t
As
ar
l
l
e
St
Early Stars
A3.4
2-
Strate
gic
Are
a4
Evolution
A4.1
Strat
egi
cA
rea
1-
sics
Phy
ar
cle
Nu
-C
Research Topics - MA1
S
t
r
a
teg
ic A
r
ea
3
-
Outline
evolution to white dwarfs
i-process
r-process
weak reactions
supernova
pipeline
How do the properties of CO white dwarfs, evolved
from the main-sequence, vary with respect to the
composite uncertainties in the reaction rates?
∑ !(reaction rates) = ?
The first Monte Carlo stellar
evolution studies that use
complete stellar models and
probability density functions
for the reaction rates.
log (Tc/ K)
8.072
8.064
3 M⊙
△M1TP = 0.02 M⊙
△t1TP = 12 Myr
△12C = 0.39
8.056
Dominate:
12
C(α,γ)
Triple-α
14
N(p,γ)
8.048
−4
A1.2
A3.5
MESA_49.net
15
Nuclear
theory
Sulfur
STARLIB rates
Phosphorus
Nuclear experiment
Silicon
JINA rates
Aluminum
Magnesium
Sodium
10
Neon
Fluorine
Oxygen
Nitrogen
Carbon
5
Observations
M Final (M⊙)
proton number
A1.1
−2
0
2
log (3α samp/ 3α med)/ log f.u.
Astrophysical
models
1.0
4
NGC 2516
NGC 3532
NGC 2287
NGC 2099
Sirius B
This Work
0.8
0.6
Boron
Beryllium
Lithium
Helium
Hydrogen
0
0
5
10
15
20
0.0
1.5
3.0
4.5
6.0
7.5
JINA-CEE enables undergraduates to be competitive for National Fellowships.
Carl Fields
2016 NSF Graduate Research Fellowship
2016 Ford Foundation Predoctoral Fellowship
See Micha Kilburn’s talk
s-process
i-process
r-process
50
82
50
28
i-process sites at low metallicity
include the He-core flash,
(S)AGB stars, and rapidly
accreting white dwarfs.
103
104
Hydrogen
burning
convective
He burn
105
1.2 M⊙
ρ
(g/cc)
Temperature
CO
106
0.6 M⊙
12
C(p,γ)13N(β+)13C(α,n)16O
22
-2
-1
PPMstar
JINA-CEE is conducting a
world-leading integrated effort
on the i-process.
Astrophysical
models
A2.1
A3.2
A3.4
A4.1
Nuclear experiment
β-Oslo technique
for (n,") with SuN
calorimeter
Observations
Ge Se
Nuclear
theory
As
Sr Zr Mo Ru Pd Cd
Rb Y Nb Tc
Te
Ba Ce NdSm Gd Dy Er Yb Hf W Os Pt Hg Pb
La Pr
Ag
Eu
Tm Lu
Ir
HD 94028
Sum of three processes
r−process
i−process
s−process
2
1
log ε
A1.6
nuclear level density +
"-ray strength function
(n,") variations increase away from stability
0
−1
−2
reliable nuclear physics is
essential for decomposition!
40
50
60
70
80
GW150914 …
… and forthcoming friends can constrain the merger rate of
neutron stars thus one promising origin site for the r-process.
range of
observing period
2
.
10
1.5ZO
ZO
0.75ZO
0.5ZO
0.25ZO
0.1ZO
.
. .
1
10
.
.
Merger Rate Density [yr−1Gpc−3]
GW150914
BH - BH
1
0
1
2
3
4
5
z
See Sanjay Reddy’s talk on EOS and
JINA-CEE is conducting an
enterprise level, consolidated
undertaking on the r-process.
A1.5
A1.6
A2.1
A3.1
A3.3
A3.4
A3.5
Neutron star merger
A4.1
Nuclear experiment
Astrophysical models
Nuclear
theory
Observations
Star 4 in Ret 2 UFD
Star in Seg 2 UFD
Relative flux
CH
100
Co(β-)70Ni
70
Intensity (%)
80
CS 22892−052 (r−process−rich halo giant)
CH
CH
CH CH CH CH
1
Zr I
Sm II
Ce II
Nd II
Zr II
Zr II
Y II
Eu II
0
60
CH
4200
4205
Ce II
Gd II
Sr II
4210
4215
4220
°)
Wavelength (A
40
Exp - SuN
Exp - SuN + Pn=7%
20
Exp - SuN uncertainty
QRPA - Moller
0
See Jason Clark’s talk on
See Tim Beer’s and Anna Frebel’s
JINA-CEE is delivering new
state-of-the-art weak reaction
data & tools to the community.
50
28
=
Z
40
N
Proton Number
50
30
50
30
40
Astrophysical
models
A1.6
A2.1
A3.1
A3.3
A3.4
A3.5
Nuclear experiment
Nuclear
theory
=
Z
28
N
Proton Number
50
40
20
30
28
82
8
20
Stable
FFN
ODA
LMP
LMSH
Approx.
No rate
20
2
10
8
2
0
0
20
www.jinaweb.org/weakrates
40
50
60
70
Neutron Number
−4
−3
80
90
Good example of a JINA-CEE triggered
and enabled student/postdoc exchange.
Nuclearspectroscopictelescopearray
NuSTAR
50
50
−5
Observations
70
60
log10|ΔYee|
20
20
20
A1.5
82
28
60
80
100
120
The Crab as an
FLASH
JINA-CEE is providing leadership
on the growth of a massive star’s
iron core, up to and including
collapse and the resulting
nucleosynthesis.
Astrophysical
models
A1.3
A1.4
A1.5
A1.6
A2.1
A3.3
A3.5
A4.1
Nuclear
theory
Nuclear experiment
Observations
NuSTAR
44Ti Mass Fraction
Injection into
protoplanetary disks
High-precision
abundances
Nucleosynthesis
Injection into
molecular clouds
Chemical evolution
Pre-solar Grains
Galaxy Hydro &
Large Scale Structure
Nuclear Physics
Stellar Model
Stellar Hydro
Modules for
Experiments in
Stellar
Astrophysics
Simple Stellar
Population Model
Stellar
Yields for
Galactic
Modeling
Applications
Galaxy Model
One-Zone
Model for the
Evolution of
GAalaxies
Merger-Tree Model
Galaxy
Assembly with
Merger-trees
Modeling
Abundances
JINA-CEE and NuGrid are leading the charge on an integrated
numerical pipeline from dynamic nuclear physics input to
transformative comparisons with observations, and loop back.
Pipeline example: following the cosmic evolution of pristine gas
FLASH
3D hydro simulations
of “primordial metals”
from Pop III SN
correlate well with
CEMP Milky Way
halo stars.
See Brian O’Shea’s talk for
Advice / Suggestions
Herwig
Truran
Van Rossum
Scielzo
Reddy
Woodward
Savard
Perdikakis
Couder
Clark
Frebel
Estrade
Aprahamian
Wiescher
Beers
Goerres
Carollo
Simon
Placco
Berg
Tan
Surman Roberston
Beard
Couch Schatz
Spyrou
O'Shea
Zegers Roederer
BrownA
Liddick
Montes
Hager
Burrows
Pignatari
Martinez-Pinedo
Brune
Froehlich
McLaughlin
Ott
Timmes
Scannapieco
Karakas
Heger
Lugaro
Mueller
Fryer
Blackmon
See Lena Simon’s talk for
additional communication results.