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Neutrino-induced production of radioisotopes in Core-Collapse - - PowerPoint PPT Presentation

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Neutrino-induced production of radioisotopes in Core-Collapse Supernovae A. Sieverding 1 , L. Huther 1 , G. Mart nez-Pinedo 1 , K. Langanke 1 , 2 ,A. Heger 3 1 Technische Universit at Darmstadt 2 GSI Helmholtzzentrum, Darmstadt 3 Monash

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SLIDE 1

Neutrino-induced production of radioisotopes

in Core-Collapse 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

MICRA 2015, Stockholm, 18th August

MICRA 2015 Neutrino Nucleosynthesis

  • A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

slide-2
SLIDE 2

Outline

1

Introduction The ν-process

2

Results with updated physics Production of 7Li,11B,19F,138La,180Ta Radioactive nuclei relevant for γ-ray astronomy Radioisotopes in meteorites

3

Summary and Outlook

MICRA 2015 Neutrino Nucleosynthesis

  • A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

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SLIDE 3

Core-Collapse Supernovae

Collapse-Collapse after hydrostatic burning turns into an explosion Hydrodynamic shock triggers explosive nucleosynthesis and ejection of material Cooling core emitts neutrinos Neutrinos influence the nucleosynthesis in outer layers of SNe

(Not to scale) from Wikimedia commons MICRA 2015 Neutrino Nucleosynthesis

  • A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

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SLIDE 4

Core-Collapse Supernovae

Collapse-Collapse after hydrostatic burning turns into an explosion Hydrodynamic shock triggers explosive nucleosynthesis and ejection of material Cooling core emitts neutrinos Neutrinos influence the nucleosynthesis in outer layers of SNe Impact on the composition of the ejecta Production of rare isotopes

(Not to scale) from Wikimedia commons MICRA 2015 Neutrino Nucleosynthesis

  • A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

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SLIDE 5

Neutrino nucleosynthesis

Emission of 1058 Neutrinos from the collapsing core Eν ≈ 8 − 13 MeV Eνe < E¯

νe ≤ Eνµ,τ

Relevant processes

1 Inverse β-decay 2 Particle emission 3 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)

MICRA 2015 Neutrino Nucleosynthesis

  • A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

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SLIDE 6

Neutrino nucleosynthesis

The supernova shock leads to high temperatures and densities Photodissociation and particle capture reactions dominate explosive nucleosynthesis ν-process affects regions with sufficient neutrino fluxes and moderate post-shock temperatures O/Ne-,C/O- and lower He-layers

MICRA 2015 Neutrino Nucleosynthesis

  • A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

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SLIDE 7

Neutrino nucleosynthesis

The supernova shock leads to high temperatures and densities Photodissociation and particle capture reactions dominate explosive nucleosynthesis ν-process affects regions with sufficient neutrino fluxes and moderate post-shock temperatures O/Ne-,C/O- and lower He-layers Main examples for the ν process:

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−)

MICRA 2015 Neutrino Nucleosynthesis

  • A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

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SLIDE 8

Neutrino Spectra from state-of-the art SN simulations

Fischer et al. (2014) Janka et al. (2012)

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

MICRA 2015 Neutrino Nucleosynthesis

  • A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

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SLIDE 9

Updated physics input

Simulations including detailed neutrino transport give new estimates for typical neutrino energies: Eν=8-13 MeV compared to 13-25 MeV Neutrino-nucleus cross-sections have been calculated for almost the whole nuclear chart (L. Huther 2014, PhD. Thesis) Parametric description of thermodynamic and neutrino-flux quantities (Woosley et al. 1990)

MICRA 2015 Neutrino Nucleosynthesis

  • A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

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SLIDE 10

Parametrization of the Supernova explosion

Parametrization of temperature and density evolution during the explosion (Woosley et al. 1990) TPeak = 2.4 × 109K × Eexpl

1051erg

1/4 ×

  • R

109cm

−3/4

Woosley et al. 2002

Neutrino flux

Exponentially decreasing neutrino luminosity Thermal Fermi-Dirac spectrum

MICRA 2015 Neutrino Nucleosynthesis

  • A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

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SLIDE 11

Outline

1

Introduction The ν-process

2

Results with updated physics Production of 7Li,11B,19F,138La,180Ta Radioactive nuclei relevant for γ-ray astronomy Radioisotopes in meteorites

3

Summary and Outlook

MICRA 2015 Neutrino Nucleosynthesis

  • A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

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SLIDE 12

Evaluation of CCSNe nucleosynthesis calculations

The solar abundances provide oberservational infomation for nucleosynthesis results to compare with

Production factor

PA = XA

X ⊙

A

Assuming that CCSNe are the main source of solar 16O : PA,normalized =

PA P16O

MICRA 2015 Neutrino Nucleosynthesis

  • A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

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SLIDE 13

Evaluation of CCSNe nucleosynthesis calculations

The solar abundances provide oberservational infomation for nucleosynthesis results to compare with

Production factor

PA = XA

X ⊙

A

Assuming that CCSNe are the main source of solar 16O : PA,normalized =

PA P16O

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

MICRA 2015 Neutrino Nucleosynthesis

  • A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

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SLIDE 14

Production factors normalized to 16O

25 M⊙ progenitor with solar metallicity (Heger et al. 2002) Nucleus no ν present work Heger et al. (2005)

7Li

10−4 0.11

  • 11B

0.003 0.8 1.18

19F

0.06 0.24 0.32

138La

0.03 0.63 0.90

180Ta

0.14 1.80 4.24 present work: Eνe = 8.8 MeV, E¯

νe,νx = 12.6 MeV

Heger et al.: Eνe,¯

νe = 12.6 MeV, Eνx = 18.9 MeV

MICRA 2015 Neutrino Nucleosynthesis

  • A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

slide-15
SLIDE 15

Outline

1

Introduction The ν-process

2

Results with updated physics Production of 7Li,11B,19F,138La,180Ta Radioactive nuclei relevant for γ-ray astronomy Radioisotopes in meteorites

3

Summary and Outlook

MICRA 2015 Neutrino Nucleosynthesis

  • A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

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SLIDE 16

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

MICRA 2015 Neutrino Nucleosynthesis

  • A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

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SLIDE 17

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

MICRA 2015 Neutrino Nucleosynthesis

  • A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

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SLIDE 18

22Na and 26Al for a set of progenitor models

15 20 25 30 35 40 Progenitor initial mass/M ⊙ 10-7 10-6 10-5 10-4 Yield/M ⊙

26 Al, without ν's 26 Al, including ν's 22 Na without ν's 22 Na, including ν's

26Al yields are modified by factors beween 1.4 and 2.2 22Na increased by factors up to 2.9

MICRA 2015 Neutrino Nucleosynthesis

  • A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

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SLIDE 19

Production channels for 26 Al

25Mg 26Mg 27Al 28Si 26Al

(ν,ν'np) (ν,ν' n) ( νe , e- ) (p,γ)

Bouchet et al. (2015)

Different mechanisms:

◮ enhancement of

p-captures

◮ charged-current channel ◮ neutral-current channels MICRA 2015 Neutrino Nucleosynthesis

  • A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

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SLIDE 20

Production of 26Al for a 15 M⊙ progenitor

1.5 2.0 2.5 3.0 Interior mass (M ⊙) 10-6 10-5 10-4 Mass fraction

a) 26 Al 15 M ⊙ star

Si-shell O/Ne-shell C/O-shell enriched in 18 O

no ν all reactions

MICRA 2015 Neutrino Nucleosynthesis

  • A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

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SLIDE 21

Production of 26Al for a 15 M⊙ progenitor

1.5 2.0 2.5 3.0 Interior mass (M ⊙) 10-6 10-5 10-4 Mass fraction

a) 26 Al 15 M ⊙ star

Si-shell O/Ne-shell C/O-shell enriched in 18 O

no ν all reactions CC only NC only

MICRA 2015 Neutrino Nucleosynthesis

  • A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

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SLIDE 22

Production of 26Al for a 15 M⊙ progenitor

1.5 2.0 2.5 3.0 Interior mass (M ) 10-6 10-5 10-4 Mass fraction Si-shell O/Ne-shell C/O-shell

no ν all reactions CC only NC only

2.26 2.28 2.30 2.32 2.34 Interior mass (M ) 2 3 4 5 6 7 Mass fraction/10−5 MICRA 2015 Neutrino Nucleosynthesis

  • A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

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SLIDE 23

Production of 22Na

21Ne 22Ne 23Na 24Mg 22Na

( νe , e- ) (p,γ) (ν,ν'np) (ν,ν' n)

Different mechanisms:

◮ indirect enhancement of

p-captures

◮ direct charged-current

channel

◮ direct neutral-current

channels

Balance of the different channels is sensitive to stellar structure and neutrino spectra

MICRA 2015 Neutrino Nucleosynthesis

  • A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

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SLIDE 24

Production of 22Na for 15 M⊙ progenitor

2.0 2.5 3.0 Enclosed mass (M ⊙) 10-8 10-7 10-6 Mass fraction Si-shell O/Ne-shell C/O-shell He-shell

22 Na

without ν

MICRA 2015 Neutrino Nucleosynthesis

  • A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

slide-25
SLIDE 25

Production of 22Na for 15 M⊙ progenitor

2.0 2.5 3.0 Enclosed mass (M ⊙) 10-8 10-7 10-6 Mass fraction Si-shell O/Ne-shell

21 Ne(p,γ)

C/O-shell

22 Ne(νe,e− )

He-shell without ν Charged-current only Neutral-current only

MICRA 2015 Neutrino Nucleosynthesis

  • A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

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SLIDE 26

Production of 22Na for 15 M⊙ progenitor

Updated ν-spectra increase the relative importance of CC reactions

2.0 2.5 3.0 Enclosed mass (M ⊙) 10-8 10-7 10-6 Mass fraction Si-shell

  • Eνx
  • =18.9 MeV
  • Eνx
  • =25.2 MeV
  • Eνx
  • =12.6 MeV

without ν s

22 Na

without ν

MICRA 2015 Neutrino Nucleosynthesis

  • A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

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SLIDE 27

Isotopic ratios from meteorites

Meteorites contain material that represents the composition of the early solar system (ESS) and the pre-solar molecular cloud A combination of nucleosynthesis events is necessary to reproduce the measured composition Isotopic ratios can be determined with high precision

Wasserburg et al (2006)

MICRA 2015 Neutrino Nucleosynthesis

  • A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

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SLIDE 28

Production of 92Nb

15 20 25 30 35 40 Progenitor main sequence mass (M ⊙) 10-12 10-11 10-10 10-9 Yield (M ⊙)

without ν

  • Eνe
  • =8.8 MeV
  • Eνe
  • =12.6 MeV

92Nb 11B 92Zr 93Nb 11B 94Mo 91Zr

34 Ma

(νe , e-)

MICRA 2015 Neutrino Nucleosynthesis

  • A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

slide-29
SLIDE 29

92Nb/93Nb ratio in the early solar system (ESS)

Assuming uniform production over 10 Gyr

15 20 25 30 35 40 Progenitor mass /M ⊙ 10-6 10-5 10-4 10-3

92 Nb/93 Nb ESS abundance ratio

Measured ESS abundance ratio without 'νs

  • Eνe
  • =8.8 MeV
  • Eνe
  • =12.6 MeV

92Nb 11B 92Zr 93Nb 11B 94Mo 91Zr

34 Ma

(νe , e-) 11B 93Zr (νe , e-)

1.6 Ma MICRA 2015 Neutrino Nucleosynthesis

  • A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

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SLIDE 30

Short-lived radionuclides from a recent event

Short-lived radioactive isotopes (10Be, 26Al, 36Cl, 41Ca, 53Mn, 60Fe) in the ESS could explained by a recent low-mass supernova

2.5 3.0 3.5 4.0 Enclosed mass/M ⊙ 10-8 10-7 10-6 10-5 10-4 10-3 10-2 10-1 Mass fraction pre-SN 36 Ar without ν including all ν reactions NC CC 15 20 25 30 35 40 Progenitor initial mass/M ⊙ 10-7 10-6 10-5 10-4 10-3 Yield (M ⊙)

36 Cl, without ν's

including νs

In the Si-shell, the production of 36Cl is increased by 36Ar(¯ νe,e+)

MICRA 2015 Neutrino Nucleosynthesis

  • A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

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SLIDE 31

Short-lived radioactive isotopes

A single event needs to reproduce the abundances of all relevant isotopes at the same time

Haxton et al. ν cross-sections (1990) Huther et al. ν cross-sections (2014) courtesy of P. Banerjee

MICRA 2015 Neutrino Nucleosynthesis

  • A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

slide-32
SLIDE 32

Summary

◮ ν nucleosynthesis affects the abundances of radioactive nuclei ◮ Important for the comparison of high-precision observations (meteorites

and γ-ray astronomy) with predicitons from simulations

◮ Uncertainties in neutrino spectra add to the uncertainties of

nucleosynthesis calculations, that can be comparable to the uncertainties due to nuclear physics.

MICRA 2015 Neutrino Nucleosynthesis

  • A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

slide-33
SLIDE 33

Summary

◮ ν nucleosynthesis affects the abundances of radioactive nuclei ◮ Important for the comparison of high-precision observations (meteorites

and γ-ray astronomy) with predicitons from simulations

◮ Uncertainties in neutrino spectra add to the uncertainties of

nucleosynthesis calculations, that can be comparable to the uncertainties due to nuclear physics.

Outlook

◮ Fallback and innermost ejecta ◮ Non-thermal and time-dependent ν-spectra ◮ Effects of neutrino oscillations MICRA 2015 Neutrino Nucleosynthesis

  • A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger

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SLIDE 34

Thank you, for your attention

MICRA 2015 Neutrino Nucleosynthesis

  • A. Sieverding, L. Huther, G. Mart´

ınez-Pinedo, A. Heger