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MA1: Stars and Stellar Explosion Models
JINA-CEE NSF Physics Frontiers Center
How do the properties of our model stars vary with respect to the composite uncertainties?
∑ 𝜹 = ?Mass resolution
Time resolution
Isotope count
Reaction rates
Mass loss
Opacity
Mixing
Yields
0100
300
Core
Mass
[%]
Solar Subsolar
-.5
0
.5
Lifetim
e
[%]
0
20
Tc
[%]
-500
50
150
ρ c [%]
-20
0
20
ξ 2.5
[%]
-3
-101
Y
He NeH C O
e
[%]
-50
0
50
Mass fra
ction
[%] 14
N22
Ne16
O16
O32
S
Fields et al 2018, 1000 MESA Monte Carlo models
See Michael Wiescher’s talk, especially on 12C(α,γ)16O
See Benoit Côté’s talk on chemical evolution.
Property 15M 20 M
M = 0 M = 0 M = 0 M
Hecore [M ]a,b 2.822.822.79 2.772.78
2.72 4.674.704.59 4.
Ccore [M ] 2.512.582.49 2.442.53
2.43 4.194.754.04 4.
Ocore [M ] 1.411.431.35 1.401.42
1.32 1.542.471.43 1.
Sicore [M ] 1.151.381.02 1.151.39
1.08 1.381.651.30 1.
Yec,Heb 0.5050.505
0.505 0.5050.5050.505 0.5050.505
0.505 0.
Yec,C 0.4990.5000.499 0.4990.500
0.499 0.4990.5000.499 0.
Yec,O 0.4990.5000.498 0.4990.500
0.498 0.4990.5000.498 0.
Yec,Si 0.4860.4980.475 0.4860.498
0.475 0.4880.4980.483 0.
∑ 𝜹 = ?
We don’t know the full answer yet, but we have useful partial answers.
Windhorst et al 2018
Pop III with JWST
! ! !"#!"#
!"#$%%&'
((((()*%+
100,000 50,0001
10
100
1,000
10,000
1 million
100,000
10 million
20,000 10,000 6,000 3,000
Temperature (K)
Lu
min
osi
ty (
L⊙)
Main Sequence
Sun with only
Hydrogen and
Helium
Hertzsprung-Russell Diagram
for the First Stars
1 M⊙
1.5 M⊙
2 M⊙
3 M⊙
5 M⊙
10 M⊙
15 M⊙
20 M⊙
30 M⊙
50 M⊙
100 M⊙
300 M⊙
1000 M⊙
6.4 Gyr
1.7 Gyr
0.7 Gyr
0.2 Gyr
70 Myr
Supernova with Black Hole
Neutron Star
White Dwarf
Supernova without Black Hole
19 Myr
11 Myr
8 Myr
6 Myr
4 Myr
3 Myr
2 Myr
2 Myr
STScI Press Release 25Apr2018
See Tim Beer’s stellar abundances talk.
Collapse after H-exhaustion
GR collapse during H-burning
Hydrostatic limit for H-burning monolithic stars
Hydrostatic limit for He-burning monolithic stars
fin
al m
ass (
10
5 M
)
accretion rate (M yr-1
)
0.3
0.4 0.5 0.6
0.8 1
1.5
2
3
0.01 0.1 1 10
Woods et al 2017Haemmerlé et al 2018a, 2018b
0.004
0.006
0.008
0.01
0.012
0.014
0.016
0.018
0.02
0.022
Radiative ignition → BH
Convective ignition → NS
16 17 18 19 20 21
Me
tall
icit
y
Mass ZAMS [M ] Petermann et al 2018
Carbon ignition
Impacts the LIGO/GAIA derived compact object initial mass function.
8 7 6 5 4 3 2 1 0
log10 FV
Ritter et al 2018
Oxygen-carbon shell mergers
3D hydro simulation → 1D diffusion coefficient → post-processing of stellar models → galactic chemical evolution.
O-shell ingestion events can be a robust site for P, Cl, K ,Sc and p-process species.
See Falk Herwig’s i-process talk.
Probing the isotopic evolution
Patton et al 2017
A ~20 kt liquid scintillator detector would typically observe ~10’s of ν in the final hours of a star’s life at 1 kpc, with ~30% from β processes.
AAS Journal highlight publication on 20Apr2018.
10 4
10 6
10 8
1010
30 M ,νe , NH, 1kpc 30M , νe, NH, 1kpc
10 4
10 6
10 8
10 10
0.010.1
Flu
xa
tE
art
h(M
eV
−1s−
1cm
−2
)F
lux
at
Ea
rth
(Me
V−1
s−1
cm−
2)
Energy (MeV)
30 M , νe , IH, 1kpc
0.010.1Energy (MeV)
30M , νe , IH, 1kpc
solarreactor
geo ν
2 h24 m
3 m2.9 m7.7 s
41 msCC
Grefenstett et al 2017
Cas A NuSTAR +
Chandra
1.5 x 10-4 M⊙
Core-Collapse SN: Low-order mode engines
Photodisintegration
αp-rich
Chasm
Normal freezeout
1D/3D Cas A
2D rotating
1D hypernova
2D MHD collapsar
α-rich freezeout
Si-rich
X(44Ti)
Peak Temperature (T9)
4104
10-2
10-3
10-4
10-5
10-6
10-7
10-8
10-9
10-10
105
106
107
108
109
1010
5 6 7 8 9 10
Pe
ak
De
nsi
ty (
g c
m-3
)
Magkotsios et al 2010
Electron-captures in supernovae
A JINA-CEE led, comprehensive library of weak reaction rates for astrophysical models.
Sullivan et al 2016
Titus et al 2018~70 nuclei in the diamond-shaped region at N~50 are drivers for changes in the p/n ratio during core-collapse. New experimental efforts are aimed at these nuclei.
See Fernando Montes’s radioactive ion beam talk.
See Sanjay Reddy’s dense matter physics talk.
0 20 40 60 80 100 120
Neutron Number
0
10
20
30
40
50
60
70
Pro
ton
Num
ber
FFN
ODA
LMP
LMSH
Approx.
No rate
2
2
8
8
20
20
28
28
50
50
82
N Z=
Stable
Number
50
R-process in jet driven supernovae
Kink unstable 3D models predict the third r-process peak is under produced.
Mösta, Roberts, et al. 2018
1600 km
See Ani Aprahamian’s r-process talk.
See Anna Frebel’s r-process talk.
Gravitational wave signals from supernovae
Morozova et al. 2018
Between ~200 and ~400 ms after bounce, the GW signal represents a g-mode. After ~400 ms the dominant GW signal is the quadrupole oscillation (l = 2, f-mode). High-frequency noise in GW spectrograms above the main signal are p-modes .
19 M⊙
Citations: 1,907
Citations to papers
that cite MESA: 19,014
Larger Science Community
MESA
InfluenceRadius ≈10 C
itations
0
150
300
450
600
2011 2012 2013 2014 2015 2016 2017 2018
MESA I 2011
MESA II 2013
MESA III 2015
MESA IV 2018
Total Citations: 1907 as of 23Apr2018
Data from SAO/NASA ADS
MESA I : Top 10 - 2011 MESA II : Top 15 - 2013 MESA III: Top 10 - 2015 MESA IV: Top 50 - 2018 $3M NSF
Pulsations:
GYRE
Stars:
Pulsations:
Adipls
MESA
Support:
MESASDK
Nuclear:
WeakLib
Cyberhub:
NuGrid
Nuclear:
StarLib
Nuclear:
AZURE3D hydro:
ENZO3D hydro:
Castro
3D hydro:
FLASH
3D hydro:
MAESTRO
3D hydro:
PPMStar
3D hydro:
Changa
3D hydro:
ATHENA
GAMMA
PyMESA
HYPATIA VMESA
MESA-Script
Support:
Data:
Support:
GCE:
Ports:
SYGMAYields:
Data:OMEGA
GCE:
Support:
JINABaseMESA-
Test
3D hydro:
Phantom
Radiation:
STELLA
N-Body:
AmuseN-body:
Amp
3D hydro:
StarCrash
Education:
MESAWeb
Support:
MESA-
Docker
Stars:
Dstar
Nuclear:
JINA
Reaclib
GAIA LSST LCO JWST NuSTAR
Isochrones:
MIST
NSCL FRIB CASPAR SECAR St. George
Critical community-driven software and data infrastructure for NSF and NASA science.