Neutrino Nucleosynthesis in the outer layers of supernovae A. - - PowerPoint PPT Presentation

Neutrino Nucleosynthesis

in the outer layers of supernovae

• A. Sieverding1, L. Huther1, G. Mart´

ınez-Pinedo1,

• K. Langanke1,2,A. Heger3

1Technische Universit¨

at Darmstadt

2GSI Helmholtzzentrum, Darmstadt 3Monash Centre for Astrophysics, Melbourne HGS-HIRe

Helmholtz Graduate School for Hadron and Ion Research

NPCSM long-term workshop Yukawa institute for Theoretical Physics 15 Nov. 2016

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Outline

1

Introduction Neutrino nucleosynthesis Review Constraints on cross-sections Supernova model

2

Results The ν process with updated physics Radioactive nuclei

3

Conclusions and Outlook

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Neutrinos and Supernovae

The core of a massive star collapses after the nuclear burning phases Collapse stops when nuclear densities are reached Hydrodynamic shock triggers explosive nucleosynthesis Cooling core emits neutrinos Neutrinos can influence the nucleosynthesis in outer layers of SNe

Schematic structure of a massive star 2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Neutrinos and Supernovae

Neutrinos are crucial for many aspects of Supernovae

1 Deleptonization and Shock

revival

◮ Neutrino signal ◮ Explosion Dynamics 2 Neutrino driven wind ◮ setting initial p/n ratio 3 ν process in the ejecta ◮ Ejecta composition ◮ Production of radioactive

isotopes

Modified, from H.T. Janka 2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Neutrino nucleosynthesis

Emission of 1058 neutrinos from the collapsing core Eν ≈ 8 − 20 MeV Eνe < E¯

νe ≤ Eνµ,τ

e+,e- p γ n α νx' p γ n α νe,νe νx A B* A A* Charged-current (CC) Neutral-current (NC)

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Neutrino nucleosynthesis

Emission of 1058 neutrinos from the collapsing core Eν ≈ 8 − 20 MeV Eνe < E¯

νe ≤ Eνµ,τ

Inverse β-decay

e+,e- p γ n α νx' p γ n α νe,νe νx A B* A A* Charged-current (CC) Neutral-current (NC)

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Neutrino nucleosynthesis

Emission of 1058 neutrinos from the collapsing core Eν ≈ 8 − 20 MeV Eνe < E¯

νe ≤ Eνµ,τ

Inverse β-decay Particle evaporation

e+,e- p γ n α νx' p γ n α νe,νe νx A B* A A* Charged-current (CC) Neutral-current (NC)

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Neutrino nucleosynthesis

Emission of 1058 neutrinos from the collapsing core Eν ≈ 8 − 20 MeV Eνe < E¯

νe ≤ Eνµ,τ

Inverse β-decay Particle evaporation Capture of spallation products

e+,e- p γ n α νx' p γ n α νe,νe νx A B* A A* Charged-current (CC) Neutral-current (NC)

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Neutrino nucleosynthesis

The supernova shock triggers photo dissociation and subsequent particle capture reactions ν nucleosynthesis occurs mainly in regions with sufficient neutrino fluxes but still moderate post-shock temperatures

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Neutrino nucleosynthesis

The supernova shock triggers photo dissociation and subsequent particle capture reactions ν nucleosynthesis occurs mainly in regions with sufficient neutrino fluxes but still moderate post-shock temperatures Main candidates for neutrino nucleosynthesis:

7Li and 11B

via 4He(νx,ν′

x p/n) and 12C(νx,ν′ x p) ...

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Neutrino nucleosynthesis

The supernova shock triggers photo dissociation and subsequent particle capture reactions ν nucleosynthesis occurs mainly in regions with sufficient neutrino fluxes but still moderate post-shock temperatures Main candidates for neutrino nucleosynthesis:

7Li and 11B

via 4He(νx,ν′

x p/n) and 12C(νx,ν′ x p) ... 19F

via 20Ne(νx,ν′

x p/n)

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Neutrino nucleosynthesis

The supernova shock triggers photo dissociation and subsequent particle capture reactions ν nucleosynthesis occurs mainly in regions with sufficient neutrino fluxes but still moderate post-shock temperatures Main candidates for neutrino nucleosynthesis:

7Li and 11B

via 4He(νx,ν′

x p/n) and 12C(νx,ν′ x p) ... 19F

via 20Ne(νx,ν′

x p/n) 138La and 180Ta via 138Ba(νe,e−) and 180Hf(νe,e−)

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Outline

1

Introduction Neutrino nucleosynthesis Review Constraints on cross-sections Supernova model

2

Results The ν process with updated physics Radioactive nuclei

3

Conclusions and Outlook

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

First ideas

ν absorption on nucleons and

4He spallation could lead to the

production of D,Li,Be,B first estimates of the relevant reaction rates

26Mg(νe,e−) as possible

mechanism to produce radioactive 26Al

4He spallation as neutron

source

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Detailed calculations

extended set of neutrino nucleus reactions detailed stellar models analytic formula for ρ(t), T(t) ∝ Tmaxe−t/τ for t ≥ t0 Tmax ∝ Eexpl

1051erg

1/4 ×

• R

109cm

−3/4 constant expansion velocity

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Neutrino-Nucleus cross sections based on shell model calculations for key nuclei (12C,16O,20Ne,24Mg . . . ) Hydrodynamic simulation of piston driven explosion

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Dedicated experiments for the determination of cross sections Detailed calculations of cross sections

• bservational constraints and uncertainties

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Neutrino Spectra from state-of-the art SN simulations

Bruenn et al. (1983) Fischer et al. (2014)

current standard

fν(Eν) ∝

1 1+exp(Eν/Tν)

◮ Eνe = 12 MeV ◮ E¯

νe = 15 MeV

◮ Eν,¯

νµ,τ = 19MeV

◮ “high ν energies”

Detailed descriptions of neutrino transport are included More channels for neutrino-matter interactions Inelastic channels reduce the average energies

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Description of ν emission

Decreasing Luminosity Lν ∝ exp

• − t

τν

• Emission of 3 × 1053 ergs

Fermi-Dirac distributed energies, Eν = 3.15 × Tν

Low ν energies

Eνe = 9 MeV(Tν = 2.8 MeV) E¯

νe = 13 MeV(Tν = 4 MeV)

Eνµ,τ = 13 MeV(Tν = 4 MeV)

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Description of ν emission

Decreasing Luminosity Lν ∝ exp

• − t

τν

• Emission of 3 × 1053 ergs

Fermi-Dirac distributed energies, Eν = 3.15 × Tν

Low ν energies

Eνe = 9 MeV(Tν = 2.8 MeV) E¯

νe = 13 MeV(Tν = 4 MeV)

Eνµ,τ = 13 MeV(Tν = 4 MeV)

High ν energies

Tνe = 4 MeV T¯

νe = 5MeV

Tν,¯

νµ,τ = 6MeV

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Realistic ν signal

5 10 15 20

• Eν
• (MeV)

νe νx ¯ νe model

2 4 6 8 10 12 14 postbounce time(s) 10-1 100 101 102 Lν (FOE/s)

νe model

ν signal from a multi-D simulation for a 27 M⊙ progenitor

• f solar metalicity provided by T.

Janka

Points for improvement:

◮ time-dependence of ν

energies

◮ burst luminosities ◮ non- Fermi-Dirac spectra 2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Outline

1

Introduction Neutrino nucleosynthesis Review Constraints on cross-sections Supernova model

2

Results The ν process with updated physics Radioactive nuclei

3

Conclusions and Outlook

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Neutrino cross sections

Two step process: Excitation and decay σk

X→Y (Eν) = i

σRPA

i

(X) × Pi(Y ) Excitation cross-section based on RPA Decay rates from Hauser-Feshbach statistical models Including emission of up to 4 particles

• L. Huther, PhD ThesisTU Darmstadt, 2014

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Neutrino-Nucleus reaction cross sections

Charged-current neutrino absorption

◮ Transitions to bound states

are most important

◮ Dominated by J = 0+ and

J = 1+ transitions

Neutral-current scattering

◮ Only particle emission is

relevant for nucleosynthesis

◮ Mainly collective excitations

at higher energies

From: Paar,Vretenar,Marketin,Ring Phys.Rev.C 77(2008) 024608 2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Cross-sections supplemented by experimental data

10-5 10-4 10-3 10-2 10-1 E 2

ν fν (

• Eν
• =12 MeV)

10 20 30 40 50 60 Neutrino energy (MeV) 100 101 102 103 cross section (10−42 cm2 )

26 Mg + νe

→

26 Al + e−

GT and Fermi transitions (data) Including forbidden transitions (RPA) Transitions to bound states, experimental Transitions to bound states

Strength for GT and Fermi transitions is experimentally accessible in

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

+ 92Zr,92Mo + 98Mo, 98Ru + 138Ba + 180T a

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Important reactions constrained by experiment

20Ne(ν,ν′),20Ne(νe,e−),20Ne(¯

νe,e+) (Anderson et al. 1991

22Ne(νe,e−) (from 22Mg decay, Hardy et al. 2003) 24Mg(ν,ν′),24Mg(νe,e−) (Zegers et al. 2008) 26Mg(νe,e−) (Zegers et al. 2005) 138Ba(νe,e−) (Byelikov et al. 2007) 180Ta(νe,e−) (Byelikov et al. 2007) 36Ar(¯

νe,e+), 36S(νe,e−) (Shell model calculations)

4He(ν , * ) (Gazit et al., (2007), Suzuki et al. (2006)) 12C(ν , * ) (Woosley et al. (1990))

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Outline

1

Introduction Neutrino nucleosynthesis Review Constraints on cross-sections Supernova model

2

Results The ν process with updated physics Radioactive nuclei

3

Conclusions and Outlook

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Supernova model

1D piston driven explosions (Heger et al. 2007) kinetic explosion energy Eexpl = 1.2 × 1051erg

0.0 0.2 0.4 0.6 0.8 1.0

Time since pre-SN (s)

0.5 1.0 1.5 2.0 2.5 3.0 3.5 4.0

piston position (1000 km)

15 M ⊙ 25 M ⊙ 13 M ⊙ 2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Supernova model

1D piston driven explosions (Heger et al. 2007) kinetic explosion energy Eexpl = 1.2 × 1051erg

0.0 0.2 0.4 0.6 0.8 1.0

Time since pre-SN (s)

0.5 1.0 1.5 2.0 2.5 3.0 3.5 4.0

piston position (1000 km)

15 M ⊙ 25 M ⊙ 13 M ⊙

Neutrino flux

Exponentially decreasing neutrino luminosity Thermal Fermi-Dirac spectrum

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

1D vs. multi-D

0.0 0.2 0.4 0.6 0.8 1.0 1.2 1.4

Time since pre SN (s)

2 4 6 8 10 12

Radius (1000 km)

Typical 1D trajectory

0.0 0.2 0.4 0.6 0.8 1.0 1.2 1.4

Time since pre SN (s)

2 4 6 8 10 12

Radius (1000 km)

2D simulation (Harris et al.) For outer layers little qualitative differences in the individual trajectories

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Updated physics in the current project

Simulations including detailed neutrino transport give new estimates for typical neutrino energies: Eν=8-13 MeV compared to 13-25 MeV Nuclear reaction data from JINA Reaclib V2.0 (2013) Lower neutrino energies put make charged-current reactions more important Neutrino-nucleus cross-sections have been calculated for almost the whole nuclear chart (L. Huther 2014, PhD. Thesis) Where available, cross-sections have been supplemented by experimental data and/or results of shell-model calculations

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Updated physics in the current project

Simulations including detailed neutrino transport give new estimates for typical neutrino energies: Eν=8-13 MeV compared to 13-25 MeV Nuclear reaction data from JINA Reaclib V2.0 (2013) Lower neutrino energies put make charged-current reactions more important Neutrino-nucleus cross-sections have been calculated for almost the whole nuclear chart (L. Huther 2014, PhD. Thesis) Where available, cross-sections have been supplemented by experimental data and/or results of shell-model calculations

Preliminary studies

Full reaction network calculations based on the analytic explosion trajectories (arXiv:1505.01082)

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Outline

1

Introduction Neutrino nucleosynthesis Review Constraints on cross-sections Supernova model

2

Results The ν process with updated physics Radioactive nuclei

3

Conclusions and Outlook

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Evaluation of CCSNe nucleosynthesis calculations

The solar abundances provide observational information for nucleosynthesis results to compare with

Production factor

PA,normalized =

• XA

X ⊙

A

• /
• X16O

X ⊙

16O

• Assuming that CCSNe are the main source of solar 16O

PA,normalized ∼ 1 indicates CCSNe as possible production site PA,normalized ≪ 1 hints another production site or mechanism

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Production factors normalized to 16O

IMF averaged production factor for 13-30 M⊙ stars (solar metallicity) Nucleus no ν Low energies1 High energies2

7Li

0.001 0.07 0.91

11B

0.005 0.45 1.81

15N

0.06 0.09 0.15

19F

0.12 0.25 0.40

138La

0.12 0.86 1.70

180Ta∗

0.6 1.49 2.67

1) Eνe = 9 MeV, E ¯

νe ,νx = 13 MeV

2) Eνe = 13MeV ,E ¯

νe = 16 MeV, Eνx = 19 MeV

*) Only about 40% of 180Ta survive in the long-lived isomeric state 2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Production factors normalized to 16O

IMF averaged production factor for 13-30 M⊙ stars (solar metallicity) Nucleus no ν Low energies1 High energies2

7Li

0.001 0.07 0.91

11B

0.005 0.45 1.81

15N

0.06 0.09 0.15

19F

0.12 0.25 0.40

138La

0.12 0.86 1.70

180Ta∗

0.6 1.49 2.67

1) Eνe = 9 MeV, E ¯

νe ,νx = 13 MeV

2) Eνe = 13MeV ,E ¯

νe = 16 MeV, Eνx = 19 MeV

*) Only about 40% of 180Ta survive in the long-lived isomeric state 2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

(Over)Production of 11B

1 Si shell 2 O/Ne shell 3 C/O shell 4 He shell

1.5 2.0 2.5 3.0 3.5 Enclosed mass/M ⊙ 10-8 10-7 10-6 10-5 Mass fraction Si mass cut O/Ne C/O He

• Eνx
• =13MeV
• Eνx
• =19MeV

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

(Over)Production of 11B

4He 3He 11B 7Be 3H 7Li

(ν,ν' p) (α,ɣ) (α,ɣ) (α,ɣ) (ν,ν' n)

8Be

53 d

11C

20 m

(α,ɣ) 1 Si shell ◮ α-rich freeze-out ◮ Spallation of 4He ◮ after the SN shock 2 O/Ne shell 3 C/O shell 4 He shell

1.5 2.0 2.5 3.0 3.5 Enclosed mass/M ⊙ 10-8 10-7 10-6 10-5 Mass fraction Si mass cut O/Ne C/O He

• Eνx
• =13MeV
• Eνx
• =19MeV

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

(Over)Production of 11B

11B 11B 12C 11C

ec (ν,ν' p/n)

12N 12B 16O

(ν,ν' α n)

1 Si shell ◮ α-rich freeze-out ◮ Spallation of 4He ◮ after the SN shock 2 O/Ne shell ◮ Production from 12C and 16O 3 C/O shell 4 He shell

1.5 2.0 2.5 3.0 3.5 Enclosed mass/M ⊙ 10-8 10-7 10-6 10-5 Mass fraction Si mass cut O/Ne C/O He

• Eνx
• =13MeV
• Eνx
• =19MeV

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

(Over)Production of 11B

11B 11B 12C 11C

ec (ν,ν' p/n)

12N

(νe,e- p)

12B

(νe,e+ n)

1 Si shell ◮ α-rich freeze-out ◮ Spallation of 4He ◮ after the SN shock 2 O/Ne shell ◮ Production from 12C and 16O 3 C/O shell ◮ Production from 12C 4 He shell

1.5 2.0 2.5 3.0 3.5 Enclosed mass/M ⊙ 10-8 10-7 10-6 10-5 Mass fraction Si mass cut O/Ne C/O He

• Eνx
• =13MeV
• Eνx
• =19MeV

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

(Over)Production of 11B

4He 3He 11B 7Be 3H 7Li

(ν,ν' p) (α,ɣ) (α,ɣ) (α,ɣ) (ν,ν' n)

8Be

53 d

11C

20 m

(α,ɣ) 1 Si shell ◮ α-rich freeze-out ◮ Spallation of 4He ◮ after the SN shock 2 O/Ne shell ◮ Production from 12C and 16O 3 C/O shell ◮ Production from 12C 4 He shell ◮ Spallation of 4He ◮ before the SN shock

1.5 2.0 2.5 3.0 3.5 Enclosed mass/M ⊙ 10-8 10-7 10-6 10-5 Mass fraction Si mass cut O/Ne C/O He

• Eνx
• =13MeV
• Eνx
• =19MeV

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Contributions to 11B production

15 20 25 Main sequence mass (M ⊙) 0.0 0.5 1.0 1.5 2.0 2.5 3.0

11 B production factor

KEPLER (Woosley 2007) high neutrino energies low neutrino energies

11B production factors

ν induced production of light ele- ments is particularly effective in low- mass low-metallicity stars (cf. Banerjee+

• Phys. Rev. Lett. 110, 141101)

14 16 18 20 22 24 26 28 30 Progenitor mass (M ⊙) 20 40 60 80 100 relative contribution to 11 B (%)

α-rich freeze-out O/Ne shell 4He shell C shell

relative contributions from different regions reflects stellar structure

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Production of 19F

Contributions from different sites AGB stars

◮ He-burning thermal pulses Lugaro et al. (2004) ◮ Observationally confirmed

Core-Collapse Supernovae

◮ Neutrino spallation ◮ shock-heated

nucleosynthesis

◮ Dominating at low

metallicity Kobayashi et al. (2011)

Wolf-Rayet stars

◮ Ejection of He-burning

material

Renda et al. (2004)

V838 Mon

Cas A

M1-67

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Production of 19F

15N 16O 17O 18O 19F

(p,α) (p,ɣ)

20Ne 19Ne

(p,ɣ)

14N 18F

(α,ɣ)

109 min

Without neutrinos:

◮ H- and He-shell burning

create regions enriched in

18O and 15N

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Production of 19F

15N 14N 16O 17O 18O 19F

(p,α) (p,ɣ) Tmax=0.6-0.7 GK

20Ne 19Ne

(p,ɣ)

18F

109 min 15N(α,ɣ)~T9.25

(α,ɣ)

Without neutrinos:

◮ H- and He-shell burning

create regions enriched in

18O and 15N

◮ High shock temperatures

enhance 15N(α,γ) and

18O(p,γ)

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Production of 19F

15N 16O 17O 18O 19F 20Ne

(ν,ν'p)

19Ne

(ν,ν'n)

14N 18F

109 min 18 s

(νe,e+ n) (νe,e- p)

Without neutrinos:

◮ H- and He-shell burning

create regions enriched in

18O and 15N

◮ High shock temperatures

enhance 15N(α,γ) and

18O(p,γ)

Neutral-current and charged-current neutrino reactions on 20Ne

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Production of 19F for a 15 M⊙ progenitor

Explosive nucleosynthesis without neutrinos

2.0 2.5 3.0 3.5 4.0 4.5 5.0 Enclosed mass/M ⊙ 10-9 10-8 10-7 10-6 10-5 10-4 10-3 10-2 Mass fraction TPeak = 0.68 GK (59 keV)

pre-SN 18 O without neutrinos

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Production of 19F for a 15 M⊙ progenitor

Including neutrino interactions

2.0 2.5 3.0 3.5 4.0 4.5 5.0 Enclosed mass/M ⊙ 10-9 10-8 10-7 10-6 10-5 10-4 10-3 10-2 Mass fraction

20 Ne(ν,ν′)

pre-SN 18 O including neutrinos

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Importance of neutrinos for the production of 19F

15 20 25 30 Main sequence mass (M ⊙) 0.0 0.1 0.2 0.3 0.4 0.5 0.6

19 F production factor

KEPLER (WH07) high energy neutrinos low energy neutrinos without neutrinos

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Using the description of the explosion as in Woosley+(1988) corresponding to an explosion energy of 1.0 × 1051 erg

10 15 20 25 30 Main sequence mass (M ⊙) 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1.0 1.1 1.2 1.3 1.4

19 F yield production factor

low energy neutrinos high energy neutrios without neutrinos

19F yields up to solar even without neutrinos

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Sensitivity to 15N(α,γ) reaction rate

2.0 2.5 3.0 3.5 4.0 Enclosed mass/M ⊙ 10-6 10-5 10-4 10-3 Mass fraction O/Ne C/O He

15 N(α,γ) from Iliadis (2010) 15 N(α,γ) from Caughlan&Fowler (1988)

Without neutrinos

◮ Yield: 7.3 × 10−5M⊙

Low energy spectrum

◮ Yield: 8.0 × 10−5M⊙

High energy spectrum

◮ Yield: 9.2 × 10−5M⊙

High energy spectrum,

15N(α,γ) from

Caughlan&Fowler

◮ Yield: 4.8 × 10−5M⊙ low energy spectra: Eνx , ¯

νe = 13MeV , Eνe = 9MeV

high energy spectra: Eνx = 19MeV , Eνe , ¯

νe = 13MeV

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Outline

1

Introduction Neutrino nucleosynthesis Review Constraints on cross-sections Supernova model

2

Results The ν process with updated physics Radioactive nuclei

3

Conclusions and Outlook

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Impact of neutrinos on the nucleosynthesis

5 10 15 20 25 30 35 40 45 50

neutron number

5 10 15 20 25 30 35 40

proton number

−2.0 −1.6 −1.2 −0.8 −0.4 0.0 0.4 0.8 1.2 1.6 2.0

log10((Yν − Yno ν)/Yno ν)

Large range of radioactive nuclei are affected

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

γ-ray astronomy

Isotope Decaytime Decay8Chain

γ γ γ γ TRay8Energy82keV3

7Be

8 778d

7Be8→

→ → → 7Li9

478

56Ni

MMM8d

56Ni8→

→ → → 56Co98→ → → →56Fe90e0

847.8M238

57Ni

39l8d

57Co→

→ → → 57Fe9

M22

22Na

3S88y

22Na8→

→ → → 22Ne9808e0

M275

44Ti

898y

44Ti→

→ → →44Sc9→ → → →44Ca90e0

MM57.878.868

26Al

MSl48Ml6y

26Al8→

→ → → 26Mg9808e0

M8l9

6lFe

2Sl8Ml6y

6lFe8→

→ → → 6lCo9

MM73.8M332

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

γ-ray astronomy

Isotope Decaytime Decay8Chain

γ γ γ γ TRay8Energy82keV3

7Be

8 778d

7Be8→

→ → → 7Li9

478

56Ni

MMM8d

56Ni8→

→ → → 56Co98→ → → →56Fe90e0

847.8M238

57Ni

39l8d

57Co→

→ → → 57Fe9

M22

22Na

3S88y

22Na8→

→ → → 22Ne9808e0

M275

44Ti

898y

44Ti→

→ → →44Sc9→ → → →44Ca90e0

MM57.878.868

26Al

MSl48Ml6y

26Al8→

→ → → 26Mg9808e0

M8l9

6lFe

2Sl8Ml6y

6lFe8→

→ → → 6lCo9

MM73.8M332

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Production of 26 Al

Well studied radioisotope

◮ By γ-ray telescopes ◮ 2.8 ± 0.8M⊙ in the

Galaxy Diehl et al. 2006

◮ in pre-solar grains ◮ 26Al/27Al ≈

10−5

Mainly from Supernovae and WR-stars Limongi&Chieffi (2006) Up to 10% contribution from AGB stars Siess&Arnould (2008)

Bouchet et al. (2015) Hynes &Gyngard (2009) 2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Production channels for 26 Al

25Mg 26Mg 27Al 28Si 26Al

(ν,ν'np) (ν,ν' n) ( νe , e- ) (p,γ)

Different mechanisms:

◮ enhancement of

p-captures

◮ charged-current channel ◮ neutral-current channels 2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

IMF averaged Yield

2.0 2.5 3.0 3.5 4.0 4.5 5.0 5.5 6.0 Enclosed mass/M ⊙ 2 4 6 8 10 12 14 16 Cumulated Yield (10−5 M ⊙)

26 Mg(νe,e− ) 25 Mg(p,γ)

additional protons e.g. 20 Ne(ν,ν' p)

24 M ⊙ star

without neutrinos high energy neutrinos

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

IMF averaged Yield

15 20 25 30 Main sequence mass (M ⊙) 5 10 15 20

26 Al yield (10−5 M ⊙)

KEPLER (WH07) high neutrino energies low neutrino energies without neutrinos

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

IMF averaged Yield

15 20 25 30 Main sequence mass (M ⊙) 5 10 15 20

26 Al yield (10−5 M ⊙)

KEPLER (WH07) high neutrino energies low neutrino energies without neutrinos

60Fe/26Al ≈ 1.25 (Observations give ≈ 0.35 )

Further contributions from less massive stars, Wolf-Rayet stars, rotating stars Isotope without ν low energy ν high energy ν

26Al

5.19 5.64 6.56

22Na

0.20 0.27 0.39

22Na with a half life of 2.6 yr is affected similarly

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Outline

1

Introduction Neutrino nucleosynthesis Review Constraints on cross-sections Supernova model

2

Results The ν process with updated physics Radioactive nuclei

3

Conclusions and Outlook

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Conclusions

◮ Study of neutrino induced nucleosynthesis for piston driven explosions

in 1D

◮ Calculations with updated neutrino energies ◮ Important neutrino-nucleus cross-sections constrained by data ◮ Detailed study of the effect on radioactive nuclei like 22Na and 26Al,

including the sensitivity to nuclear reactions rates

2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

Conclusions

◮ Study of neutrino induced nucleosynthesis for piston driven explosions

in 1D

◮ Calculations with updated neutrino energies ◮ Important neutrino-nucleus cross-sections constrained by data ◮ Detailed study of the effect on radioactive nuclei like 22Na and 26Al,

including the sensitivity to nuclear reactions rates

Outlook

◮ Cross sections based on QRPA ◮ Tracer particles from multi-D SN simulations ◮ Take into account time-dependent,non-Fermi-Dirac neutrino spectra 2016 Neutrino Nucleosynthesis

• A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger