H & He Burn

PyconuclearMA2 MA1

Masses

Neutron Capture

Transport

X-ray Burst

Superburst

NS Mergers

X-ray LC

X-raySpectra

NS Crust NS

Nuclear

H-BurnHe-Burn

C-Burn

Screening

Weak Reactions

Neutron Production

Observations

First Stars

i-process

r- and νp-process

Early Stars

SupernovaeChem Evol

Nuclear PhysicsAstrophysi

cal M

odel

sO

bservations

JINA-CEE NSF Physics Frontiers Center

MA1 Strategic Areas

A1: Provide the new experimental and theoretical nuclear physics needed to quantitatively assess the contributions of individual nucleosynthesis events.

A2: Obtain heavy-element abundance data for chemically-primitive stars in the Local Group of galaxies.

A3: Construct state-of-the-art astrophysical models that quantitatively predict nucleosynthesis contributions from stars and supernovae.

A4: Integrate the nuclear physics, stellar abundance determinations, and stellar nucleosynthesis yields into classical and modern chemical-evolution models.

JINA-CEE NSF Physics Frontiers Center

See Michael Wiescher’s, Artemis Spyrou’s, and Sanjay Reddy’s talks

See Falk Herwig’s and Anna Frebel’s talks

See Tim Beer’s and Anna Frebel’s talks

See Falk Herwig’s and Gail McLaughlin’s talks

MA1 Community Network

Member Institution

UMichiganLBL

LLNL

Al-BalqaU

Texas A&MLSU

Knoxville

Vanderbilt

MPI-ET TU-DarmstadtHull Frankfurt ChETEC

Core Institution

MSU

ASU

UW

ND

Caltech

TRIUMFUVictoria

Monash

Sao Paulo

Princeton

MITUConn

NC State

Ohio State

Stony Brook

UMinnesota

UChicagoWMichigan

CentMi

Argonne

Urbana

LANL

Working Groups

Institutions

344

12C+12C and Super Asymptotic Giant Branch Stars

Modules for Experiments in Stellar Astrophysics (MESA)

First 3D simulation of the final minutes of iron core growth in a massive star, up to and including core-collapse

First 3D GRMHD simulation of a core-collapse supernova driven by rapid rotation and strong magnetic fields

r-process variations with nuclear mass model

First 3D simulations of He-shell flash convection with proton-rich fuel entrainment

First converged 3D simulations of double WD mergers and collisions

First 3D simulations of mixing of radionuclides into molecular clouds

First 3D simulations of primordial metals generated and mixed by the first supernovae correlate well with CEMP halo stars

Chemical evolution informed from 3D cosmological simulations

r-process origin sites from neutron star mergers

First Monte Carlo stellar evolution models exploring the impact of the experimental uncertainties in reaction rates

Survey nuclear level density and gamma-ray strength function options in TALYS Hauser-Feshbach models

β-Oslo technique for indirect extraction of (n,γ) rates

i-process nucleosynthesis and contributions to chemical evolution

Neutron star merger rates from LIGO and chemical evolution models

Measurement of (α,n) reactions or weak r-process sensitivity

Constrain electron-capture rates via (t,3He) and 56Ni(p,n)

JINA-CEE Weak Interaction Library

New 20Ne(e−,𝝂)20F rates and electron-capture supernova

NASA NuSTAR correlating JINA 44Ti and 56Ni results

New helium burning rates from stable beam experiments and R-matrix analysis

Nugrid yields from non-rotating 1D stellar evolution models

First 3D simulations of carbon-oxygen shell mergers; a robust site for P, Cl, K ,Sc and p-process species

Discovery: CEMP-no stars hold the nucleosynthesis of the first stars

Discovery: Highly r-process enhanced stars in Reticulum II

JINA NuGrid chemical evolution pipeline

Chemical cartography, e.g., carbon maps of the Milky Way.

New measurement of 12C+16O and 12C+12C in concert with theoretical and observational studies

Observing the first stars with the James Webb Space Telescope

Origin of the first supermassive black holes

Probing the isotopic evolution of massive stars with pre-SN 𝜈

First 3D simulations of r-process in jet driven supernovae

Gravitational wave signals from 3D supernovae simulations

Cyberhubs: Virtual Research Environments for Astronomy

Impact of white dwarf luminosity profiles on oscillation frequencies

5 years of presented major achievements

Hypatia compilation of chemical abundances of nearby stars

JINAbase compilation of chemical abundances of metal-poor stars

Catching element formation in the act

JINA reaclib for nuclear reaction rates

JINA AZURE R-matrix software instrument

Mapping helium burning

Exploring nucleosynthesis of first stars

Nuclear Physics

Observations

Astrophysicsmodels

First Monte Carlo stellar evolution models exploring the impact of the experimental uncertainties in reaction rates. Originated, motivated and led by JINA-CEE.

Fields et al 2018

0.6 0.8 1.0 1.2 1.4

Rate Multiplier @ Max f.u.

11.24

11.26

11.28

11.30

τTAMS(M

yr)

Tc

62.0

62.5

63.0

63.5

64.0

Tc(M

K)

14N(p,g)15O

Solar @ H Depletion

τTAMS

0.3 0.6 0.9 1.2 1.5 1.8

T (GK)

1.0

1.1

1.2

1.3

1.4

1.5

1.6

fact

or

un

cert

ain

ty

He C Ne O

12C(a,g)16O14N(p, g)15O23Na(p, a )20Ne

Triple-alfa

0. 0 1. 5 3. 0 4. 5 6. 0 7. 5

Initial (M⊙M )

0.6

0.8

1.0

Fin

al(M

⊙M

)

NGC 2516

NGC 3532

NGC 2287

NGC 2099

Sirius B

This Work

1153 modelslow, medium, high rates

PARSEC isochronesfor observations

Fields et al 2016

Fields et al 2018

See Michael Wiescher’s talk

See Falk Herwig’s talk

A research outcome attributed to the existence of the Center.

Nuclear Physics

ObservationsAstrophysical

models

New insights in heavy element nucleosynthesis - the i-process.

An intermediate neutron-capture process that occurs in convective-reactive environments. Originated, motivated and led by JINA-CEE.

Jones et al. 2016 Roederer et al. 2016See Falk Herwig’s talk

See Anna Frebel’s talk

See Artemis Spyrou’s talk

A Center enabled breakthrough at the intellectual frontier.

SuN detector,β-Oslo

Atomic Number

[X/F

e]

40 50 60 70 80

0

1

2

GeAs

SeRb

SrY

ZrNb

MoTc

Ru PdAg

Cd Te BaLa

CePr

NdSmEu

GdDy ErTm

YbLu

Hf W OsIr

Pt Hg Pb

HD 94028Sum of three processesr−processi−processs−process

PPMStar

Nuclear PhysicsGalaxy Hydro &

Large Scale Structure

Stellar Hydro

Stellar Model

StellarYields forGalacticModelingApplications

Modules forExperiments inStellarAstrophysics

One-ZoneModel for theEvolution of GAalaxies

GalaxyAssembly withMerger-treesModelingAbundances

Galaxy Model Merger-Tree ModelSimple StellarPopulation Model

Nuclear Physics

ObservationsAstrophysical

models

New insights in heavy element nucleosynthesis - the r-process. JINA-CEE is in a unique position to assess the nuclear physics of neutron star mergers and other sites for explaining the origin of the heavy elements.

Star 4 in Ret 2 UFD

CH

Zr I

0

1

4200 4205 4215 4220

Wavelength (Å)

Rel

ativ

e fl

ux

4210

Zr II Zr IICe II Ce IIGd II

Sr II

Sm II

Y II Eu II

Nd II

CH CH CH CH CH CH CH

Star in Seg 2 UFD CS 22892-052 (r-process-rich halo giant)

Roederer et al. 2016

Mumpower et al. 2017

Mösta, Roberts, et al. 2018

See Tim Beers’ talk

See Sanjay Reddy’s talk

See Gail McLaughlin’s talk

Research that could not have been done without the Center.

New

Fro

ntiers

3 rd peak 2n

d pea

k

1st p

eak Theory and Models

Mul

ti-m

esse

nger

Obs

erva

tion

s

Experiment

r-process

Chairs: Timmes, Mohammad Safarzadeh , Evan Scannapieco

2002

2014

FO

2008

2001

JINA

Frontiers of Nuclei

JINA-CEERise of the Elements

Dynamic Nucleosynthesis

JINA-2

Nuclei of the Cosmos

J I N A

Windhorst et al 2018

Frontiers: First stars 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)

Lum

ino

sity

(L⊙)

Main Sequence

Sun with onlyHydrogen and

Helium1 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 Gyr1.7 Gyr

0.7 Gyr

0.2 Gyr

70 Myr

Supernova with Black Hole

Neutron Star

White Dwarf

Supernova without Black Hole

19 Myr

11 Myr8 Myr

6 Myr

4 Myr

3 Myr

2 Myr

2 Myr

Explore the impact of 3He(α, γ)7Be, 7Li(α, γ)11B, 11B(α,n)14C, 10B(α,n)13N and 10B(p,α)7Be in zero-metal stellar models in concert with new experimental studies.

Survey the impact of close binary systems on nuclear burning and stellar evolution.

Supplemental Proposal: This activity effectively continues the Center’s impacts.

Y6 FO

0.00 0.25 0.50 0.75 1.00

Mr /M

1.00

0.75

0.50

0.25

0.00

MassFraction Oxygen

Carbon

Helium

Timmes et al 2018, 2019

Frontiers: Nucleosynthesis and Asteroseismology

Combine new asteroseismology data (Kepler, TESS, and PLATO) with stellar evolution to constrain challenges in the origin of the elements.

For example, determine the effective 12C(α, γ)16O reaction rate from the low-order g-mode frequencies observed in carbon-oxygen white dwarfs.

Supplemental Proposal: This activity extends the Center’s ecosystem and impacts.

Y6 FO

Catching Element Formation In The Act

The Case for a New MeV Gamma-Ray Mission:Radionuclide Astronomy in the 2020s

A White Paper for the 2020 Decadal Survey

AuthorsChris L. Fryer, Los Alamos National Laboratory, fryer@lanl.gov, (505) 665-3394Frank Timmes, Arizona State University, fxtimmes@gmail.com, (480) 965-4274

Aimee L. Hungerford, Los Alamos National LaboratoryAaron Couture, Los Alamos National Laboratory

Fred Adams, University of MichiganWako Aoki, National Astronomical Observatory of JapanAlmudena Arcones, Technische Universitat Darmstadt

David Arnett, University of ArizonaKatie Auchettl, DARK, Niels Bohr Institute, University of Copenhagen

Melina Avila, Argonne National LaboratoryCarles Badenes, University of PittsburghEddie Baron, University of Oklahoma

Andreas Bauswein, GSI Helmholtzzentrum fur SchwerionenforschungJohn Beacom, Ohio State University

Jeff Blackmon, Louisiana State UniversityStephane Blondin, CNRS & Pontificia Universidad Catolica de Chile

Peter Bloser, Los Alamos National LaboratorySteve Boggs, UC San Diego

Alan Boss, Carnegie Institution for ScienceTerri Brandt, NASA Goddard Space Flight Center

Eduardo Bravo, Universitat Polit` ecnica de CatalunyaEd Brown, Michigan State UniversityPeter Brown, Texas A&M University

Steve Bruenn, University of Florida AtlanticCarl Budtz-Jørgensen, Technical University of Denmark

Eric Burns, NASA Goddard Space Flight Center, Universities Space Research AssociationAlan Calder, Stony Brook University

Regina Caputo, NASA Goddard Space Flight Center

225 co-authors; enabled by JINA-CEE

This activity extends the Center’s ecosystem and impacts.

Y6 FO

Citations: 2,456

Citations to papersthat cite MESA: 37,645

Larger Science Community

MESA

InfluenceRadius ≈15

MESA I - Top 5 in 2011 MESA III - Top 5 in 2015

MESA IV - Top 30 in 2018 MESA II - Top 10 in 2013

Cita

tions

0

300

600

900

2011 2012 2013 2014 2015 2016 2017 2018

MESA I 2011MESA II 2013MESA III 2015MESA IV 2018

Data from SAO/NASA ADS

A JINA-CEE leveraged activity that broadens opportunities and expands participation to the larger science community.

Y6 FO

JINA-CEE enables community-driven instruments and people that accelerate science and discovery.

PPMStar

WENDI

OMEGA

SYGMA GAMMA

ENZO

FLASH

MESA GYRE

AZURE

JINAbaseHypatia

REACLIB STARLIB WEAKLIBNuclear:

Nuclear: Nuclear: Nuclear:

Chem evol:

Chem evol: Chem evol:

Chem evol:

Observe: Observe:

Stars:

Stars:

Stars:

Stars:

Community:Community:

Community:

Galaxies:

JINA-CEEChETEC

NuGrid

LIGO Hubble NuSTARGaia SDSS JWST TESS

NSCL FRIB CASPAR SECAR St. George