r-process theory and the connections to nuclear physics

Rebecca SurmanUniversity of Notre Dame

JINA Horizons

1 December 2020

R Surman, JINA Horizons 1 Dec 20

rapid neutron capture (r-process) nucleosynthesis: the astrophysical formation of the heaviest elements

simulation by E Holmbeckwith PRISM (Sprouse/Mumpower)

Reichert+2020also Nishimura+2017; Mösta+2018

Nedora+2020also, e.g., Foucart+2020; George+2020; Camelio+2020; Law-Smith+2020; Hayashi+2020

r-process astrophysical sites

R Surman, JINA Horizons 1 Dec 20

NS-NS/NS-BH mergersMR-SNe

e.g., Siegel+2019, Miller+2019

e.g., Fuller+2017

e.g., Fischer+2020

collapsars

PBH-NS

exotic SNe

etc.

see talks by B Côté, A Skuladottir

R Surman, JINA Horizons 1 Dec 20

AME 2016FRIB Day 1 reachFRIB design goal

r-process studies with next-generation nuclear experiment and theory

see talks by A Spyrou, J Clark, R Reifarth, I Dillmann, A Lowell

10−1 100 101 102 103

Time (Day)

1037

1038

1039

1040

1041

1042

1043

Effective

HeatingRate(erg

s−1)

FRDM2012

HFB27

HFB22

WS3

DZ33

SLY4

UNEDF1

ETFSI

TF

TF+D3C*

Zhu, Lund+2020

also Barnes+2020; Even+2019; Hotokezaka, Nakar 2020; Korobkin+2020; Fujimoto, Hashimoto 2020; Banerjee+2020; Kawaguchi+2020; Giuliani+2020

R Surman, JINA Horizons 1 Dec 20

see talk by J Barnes

r-process electromagnetic signatures: kilonovae

R Surman, JINA Horizons 1 Dec 20

Wang,Vassh+2020: gammas from fissioning isotopes

Korobkin+2020also Hotokezaka+2016; Li 2019; Wu+2019; Ruiz-Lapuente, Korobkin 2020

see talk by C Fryer

r-process electromagnetic signatures: gamma rays

key isotopes for electromagnetic signatures

R Surman, JINA Horizons 1 Dec 20

154 156 158 160N

Cm

Bk

Cf

Es

Fm

Md

Z

10°16

10°14

10°12

10°10

10°8

10°6

Abundan

ce

b-decay contributions

to KN heatingZhu, Lund+2020

also Hotokezaka+2020

Cf-254Zhu+2018

also Wu+2019

astromersMisch+2020, also Fujimoto, Hashimoto 2020

r-process abundance patterns

Arnould+2007, Hotokezaka+2018

solar system r-process residuals

elemental abundances from r-process-enhanced

metal-poor stars

Holmbeck+2020

R Surman, JINA Horizons 1 Dec 20

see talk by T Hansen

rare earth peak: a window into r-process dynamics

Vassh+2020

R Surman, JINA Horizons 1 Dec 20

reverse-engineered nuclear mass predictions for three types of

astrophysical environments compared to experimental data

nsm properties from metal-poor star elemental ratios

Holmbeck+2020

R Surman, JINA Horizons 1 Dec 20

40 50 60 70 80 90Atomic Number (Z)

10°8

10°6

10°4

10°2

Abundan

ce

Zr

Dy Th

Solar r

Dynamical

0 ms

10 ms

100 ms

1

0.1

1

10

120 140 160 180 200

0.1

1

10

0.1

1

10

Y(A

)Ym

ean(A

)

A

0.1

1

10

120 140 160 180 200

(c)

Y(A

)Ym

ean(A

)

0.1

1

10 (b)

Y(A

)Ym

ean(A

)

0.1

1

10 (a) high entropy wind

low entropy wind

nsm dynamical ejecta

prospects with next-generation radioactive ion facilities

Sprouse+2019

R Surman, JINA Horizons 1 Dec 20

nucleosynthesis tracing

Movie by Trevor Sprouse, from Sprouse, Mumpower, Surman, arXiv:2008.06075

130 140 150 160 170 180 190 200 210

A

10°6

10°5

10°4

10°3

Y(A

)

152Nd176Nd186Nd

2020 has seen rapid progress in many areas of r-process science. Still, the origins of r-process nuclei in our galaxy remain elusive.

The interpretation of r-process observables is complicated by numerous uncertainties, including in the nuclear physics of the thousands of nuclei that participate in the r process.

The next generation of radioactive beam facilities offers great promise to dramatically reduce these uncertainties. To realize this promise will require:• the development and refinement of innovative diagnostics of r-process

environments based on key observables: electromagnetic signals, abundance patterns and ratios, solar system radioactivities

• community efforts to identify the highest impact measurements connected to these diagnostics and support of the relevant experimental proposals

summary

R Surman, JINA Horizons 1 Dec 20