carla fröhlich north carolina state universitycompact-merger.astro.su.se/micra2015/slides/... ·...
TRANSCRIPT
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Setting the stage: Nucleosynthesis
Carla FröhlichNorth Carolina State University
18 August 2015MICRA Workshop
North Carolina State University
Together with students and collaborators
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Outline
• Introduction
• Core-collapse supernovae
• Heavy elements: r-process, LEPP process• Heavy elements: r-process, LEPP process
• X-ray bursts (afternoon discussion)
2
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Nucleosynthesis: Goals
r-process
s-process
νp-process
rp-process
p-process
3
We want to understand:• Abundance distribution in our Sun• Abundance distribution in metal-poor stars• Nuclear processes synthesizing elements
Stellar burning
Explosive burning
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Nucleosynthesis: Goals
r-process
s-process
νp-process
rp-process
p-process
Astrophysical sites:• Stellar evolution of low-mass
and massive stars• AGB stars (main s-process)• core He-burning of massive
stars (weak s-process)• Supernovae• Core-collapse supernovae• Core-collapse supernovae• Neutrino-driven winds in SNe?
4
We want to understand:• Abundance distribution in our Sun• Abundance distribution in metal-poor stars• Nuclear processes synthesizing elements
Stellar burning
Explosive burning
• Neutrino-driven winds in SNe?NS mergers
• X-ray bursts
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Nucleosynthesis: Goals
Ma
ss
5
We want to understand:• Abundance distribution in our Sun• Abundance distribution in metal-poor stars• Nuclear processes synthesizing elements• Chemical evolution
Time
[Fe/H]
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Outline
• Introduction
• Core-collapse supernovae
• Heavy elements: r-process, LEPP process• Heavy elements: r-process, LEPP process
• X-ray bursts (afternoon discussion)
6
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Core-collapse supernovae
7
Core bounce(max compression) Explosion
ν-emission
Stellar burning� C, O
Weak s-process� heavy elements
Explosive burning� Si, S, Ca, Fe, Ni, Zn
νp-rpocess� Sr, Y, Zr + Mo, Ru
r-process ???γ-process
� p-nuclides
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Core-collapse SNe
8
Open questions in SN simulations and nucleosynthesis:
• Explosion mechanism: Nucleosynthesis predictions
depend on explosion mechanism
• Conditions in the neutrino-driven wind: neutron-rich or
proton-rich or both?
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Simulations of core-collapse SNe
• Status of ccSN simulations:
• Spherically symmetric simulations with detailed
neutrino-transport fail to explode
(except for lowest mass progenitors)
• Many ongoing efforts in 2D and 3D
• Qualitative and quantitative differences
• Computationally expensive
Oak Ridge
Couch / O’Connor MPA
Basel
+ manymore!
� See Friday talks
• Computationally expensive
� too expensive for systematic studies of large
numbers of progenitors
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Simulations of core-collapse SNe
• But: want to address questions such as
• What are conditions for explosive nucleosynthesis?
• Connection between progenitor and remnant?
• How are they related to explosion dynamics and
energetics?
• Nucleosynthesis predictions (also for GCE)
• How to predict CCSN nucleosynthesis if multi-D
models are still on their way?
• Need induced explosions
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Induced explosions
• Example: Piston / thermal bomb models
• initiate explosion by increasing temperature or
placing a piston in the pre-collapse star
• Limitations: physics of collapse, bounce, and onset of
explosion; no neutrinos; cannot predict Ni yields
11
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Nucleosynthesis
• Effects of induced explosion method on
nucleosynthesis
56Ni58Ni
fra
ctio
n
M(r)
Frohlich+(2006a)
Ye: e
lectr
on
fra
ctio
n
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A new method: PUSH
• Mimic multi-D effects using mu/tau neutrinos
(PUSH)
• Provide extra energy deposition in heating region
from mu/tau neutrinos in otherwise consistent
simulation (hydro + neutrino transport + EOS + GR)
• Prescribe location and dependency on luminosity• Prescribe location and dependency on luminosity
• Parameters determination:
• Use multi-D simulations for typical timescales
• Use SN1987A for strength of PUSH
Seitenzahl+14Fransson & Kozma 02
Woosley98; Shigeyama &Nomoto90
Blinnikov+00
Perego, Hempel, CF+ (2015)
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SN1987A
Perego, Hempel, CF+ (2015)
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SN1987A (with fallback)
Perego, Hempel, CF+ (2015)
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Nucleosynthesis
• 57Ni and 58Ni:
• Produced in slightly neutron-rich layers with alpha-
rich freeze-out
• Required conditions found in Si-shell
• location of transition from Si-shell to O-shell with
respect to final mass cut mattersrespect to final mass cut matters
• If transition is inside mass cut: low 57,58Ni production
Perego, Hempel, CF+ (2015)
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Nucleosynthesis
• 57Ni and 58Ni:
• Produced in slightly neutron-rich layers with alpha-
rich freeze-out
• Required conditions found in Si-shell
• location of transition from Si-shell to O-shell with
respect to final mass cut mattersrespect to final mass cut matters
• If transition is inside mass cut: low 57,58Ni production
• 44Ti:
• Produced in the innermost 0.15Msun
• Uncertainties due to uncertainties in rates of 40Ca(α,γ) 44Ti and 44Ti(α,p) 47V
• Homogeneous mixing + new rate for 44Ti(α,p) +
fallback: 3.99e-5Msun of 44Ti
Margerin+14
Perego, Hempel, CF+ (2015)
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Compact remnant of SN1987A
• From observational side: still obscure
• Neutrino signal: formation of PNS for at least 12s
• Our prediction for NS mass: 1.66Msun
• BH formation: unlikely
• Would require additional 0.5-1.3Msun of fallback to
exceed max mass predicted by HS(DD2) EOS
• Difficult to match observational properties and form BH
• Unlikely in 2D simulation of 15Msun progenitor
• Pulsar: unlikely (from HST observations) but our
simulations would be consistent with a NS with
very low magnetic field
Kifonidis+06
Graves+05
Perego, Hempel, CF+ (2015)
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Core-collapse SNe
19
Open questions in SN simulations and nucleosynthesis:
• Explosion mechanism: Nucleosynthesis predictions
depend on explosion mechanism
• Conditions in the neutrino-driven wind: neutron-rich or
proton-rich or both?
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Neutrino-driven winds
• Strong neutrino flux
from PNS
• Drives matter-outflow
behind shock wave
• Nucleosynthesis:
Figure: Janka
• NSE (T=10-8GK)
• Charged-particle reactions
(8-2GK)
• r-process and νp-process
nucleosynthesis (3-1GK)
Conditions in wind determine details of nucleosynthesis(Ye, entropy, timescale)
Fig
ure
: B
ruenn
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Conditions in neutrino-driven winds
• Electron fraction Ye: set by weak interactions
• Luminosity ratio
• Difference in neutrino energies:
• Proton-rich if
• Details of microphysics treatment in EOS
(in medium effects, e.g.)
• Entropy s: 50-120 kB/nuc in recent SN
simulations (� no full r-process)
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Proton-rich ejecta
PUSH method
MPA group ORNL group
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Proton-rich ejecta
• What nucleosynthesis is possible in proton-rich
neutrino-driven winds?
• hydrodynamics / reverse shock
• Neutron-rich winds
• Nuclear physics:
Arcones, Frohlich, Martinez (2012)Wanajo et al (2012)
Arcones & Montes (2011)Bliss+ (2014)
• Nuclear physics:
• trajectory independent predictions of critical inputs
• Nuclear masses I � affect abundances locally
• Nuclear masses II � new experimental efforts a
Lanzhou
• Nuclear reactions � experimental efforts
Frohlich & Rauscher (2012)
Weber et al (2008)
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The νp-Process
• proton-rich matter is ejected
under the influence of neutrino
interactions
• true rp-process is limited by
slow β decays, e.g. τ(64Ge)
• Neutron source: Fro
hlic
he
t a
l (2
00
6)
• Antineutrinos help bridging long
waiting points via (n,p)
reactions:64Ge (p,g)
(n,p)
64Ge (n,p) 64Ga64Ga (p,γ) 65Ge
(n,p)
(p,g)
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The νp-Process
• proton-rich matter is ejected
under the influence of neutrino
interactions
• true rp-process is limited by
slow β decays, e.g. τ(64Ge)
• Neutron source: Fro
hlic
he
t a
l (2
00
6)
• With neutrinoso Without neutrinos
• Antineutrinos help bridging long
waiting points via (n,p)
reactions:64Ge (p,g)
(n,p)
64Ge (n,p) 64Ga64Ga (p,γ) 65Ge
(n,p)
(p,g)
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Effect of Mass Measurements
• Same hydrodynamic profile• Only reaction rates are different
88Tc
This
work
: W
eber
et al (2
008)
[31]:
Kankain
en
et
al (2
006)
Masses:• enter rate calculations• Change proton-separation energy• Change Q-value� reverse rate ~exp(-Q/kT)
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Reaction rates for nucleosynthesis
• All important reaction rates from Hauser-
Feshbach predictions
� What is impact of uncertainties?
• Reactions on light nuclei Wanajo et al (2012)
• 56Ni(n,p);
• Seed nucleus for νp-process but also neutron poison
• 64Ge(n,p):
• Bottle neck
• 96Pd(n,p):
• Predicted as second seed, but not confirmed
Wanajo et al (2012); Frohlich+ (2012)
Frohlich+ (2012)
Frohlich+ (2012)
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Systematic sensitivity study
• Systematically vary each reaction rate
individually for all nuclei from Ni to Sn and
from N=Z to first stable isotope
• Reaction types: (n,p), (n,g), (p,g)
• Factors: 10 and 0.1
• Conditions: 2 different νp-process trajectories
Fro
hlic
h&
Hatc
her
(2015)
• Conditions: 2 different νp-process trajectories
(“standard” and “strong”)
(n,p) reactions:• Accelerate matter flow to heavier nuclei• Several individual reactions are important, mostly in even Z
and close to N=Z
Fro
hlic
h
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Outline
• Introduction
• Core-collapse supernovae
• Heavy elements: r-process, LEPP process• Heavy elements: r-process, LEPP process
• X-ray bursts (afternoon discussion)
29
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Heavy element nucleosynthesis
• What conditions are needed to explain
observed abundances?
Figure: John Cowan Roederer 2013
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Observational constraints
31Roederer 2013
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LEPP: Lighter Element Primary Process
• Observations of halo stars indicate two “r-
process” sites:
• Main r-process
• Stellar LEPP / weak r-process
32
Stars with high enrichment in heavy r-process abundances
Stars with low enrichment in heavy r-process abundances
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Neutron-capture processes
heavy elements are
made by
slow (τβ/τn<1)
and
fast (τβ/τn>1)
• Sequences of (n,g) reactions and β—decays
• Closed neutron-shells give rise to the peaks at
Te,Xe / Ba and at Os,Pt,Au / Pb
β n
neutron-capture events
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The r-process
r-process path1st peak: A~80 (N=50)2nd peak: A~130 (N=82)3rd peak: A~195 (N=126)
Primary process!
Stable nuclei
iron Silver
Gold
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Conditions for the r-process
• High entropy, alpha-rich freeze-out
• Low entropy, normal freeze-out with very low Ye
35
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The r-process site(s)
• Neutrino-driven wind in CCSNe
Arcones, Burrows, Janka, Farouqi, Hoffman, Kajino, Kratz, Martinez-Pinedo, Mathews, Mahler, Meyer, Qian, Takahara, Takahashi, Thielemann, Thompson, Wanajo, Woosley, ….
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Wind conditions for r-process
• High neutron-to-seed ratio: Yn/Yseed ~ 100
• Short expansion timescale: 10-3 to 1 second
� inhibits formation of nuclei through α-process
• High entropy: s/kB ~ 20 – 400
� many free nucleons
• Moderately low electron fraction: Ye<0.5
37
BUT: Conditions not realized in recent simulations
Simulations find:τ ~ few millisecondss ~ 50-120 kB/nucYe ~ 0.4 – 0.6
� Additional ingredients??
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The r-process site(s)
• Neutrino-driven wind in CCSNe
• ONeMg core collapse
• Quark-hadron phase transition
If? Weak!
weak
No?!
???
Wanajo & Janka
Nishimura, Fischer, CF, Thielemann
• Explosive He-burning in outer shells
• Charged-current neutrino interactions
in outer shells
• Polar jets from rotating CCSNe
Abundance pattern??
Cameron, Fujimoto, Käppeli, Liebendörfer, Nishimura, Takiwaki, Thielemann, Winteler, Mösta, Ott
Cameron, Cowan, Truran, Hillebrandt, Thielemann, Wheeler, Nadyozhin, Panov, CF
Haxton, Qian, Banerjee
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Magnetorotational SNe
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Nucleosynthesis from rot. CCSNe
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Effects on abundance pattern
Mass model Fission yield distribution
41Eichler+ (2014, 2015)
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3D Study (Mösta+ 2014)
42� Talk by Philipp Mösta
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Rotation rates and magn fields
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The r-process site(s)
• Neutrino-driven wind in CCSNe
• ONeMg core collapse
• Quark-hadron phase transition
• Explosive He-burning in outer shells
• Charged-current neutrino interactions
If? Weak!
weak
No?!
???
• Charged-current neutrino interactions
in outer shells
• Polar jets from rotating CCSNe
• Neutron-star mergers
• BH accretion disks
Abundance pattern??
Promising;initial conditions??
Freiburghaus, Goriely, Janka, Bauswein, Panov, Arcones, Martinez-Pinedo, Rosswog, Argast, Korobkin, Wanajo, Just, Martin, Perego
� Talk by Albino Perego; also Korobkin
McLaughlin, Surman, Wanajo, Janka, Ruffert, Perego
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Strong r-process: contributing events?
NS mergers and/or rotational CCSNe?
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Neutron-star mergers
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Neutron-star mergers
• 3rd peak always shifted to heavier nuclei
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Neutron-star mergers
• 3rd peak always shifted to heavier nuclei
• Due to late-time neutron captures after freeze-out of
(n,g)-(g,n) equilibrium
Effects of … on peak location:
• Mass formula
• fission barriers and yield distribution
Eichler+ (2014, 2015)Petermann+ (2012)Korobkin+ (2012)Caballero+ (2014)Marketin+ (2015)Panov+ (2014)• fission barriers and yield distribution
• Rates (beta-decays, fission)
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Panov+ (2014)Mendoza-Temis+ (2014)Shibagaki+ (2015)
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Neutron-star mergers
• 3rd peak always shifted to heavier nuclei
• Due to late-time neutron captures after freeze-out of
(n,g)-(g,n) equilibrium
Effects of … on peak location:
• Mass formula
• fission barriers and yield distribution
Eichler+ (2014, 2015)Petermann+ (2012)Korobkin+ (2012)Caballero+ (2014)Marketin+ (2015)Panov+ (2014)• fission barriers and yield distribution
• Rates (beta-decays, fission)
• Problem is not the nuclear physics, but
trajectories are too neutron-rich
• GR simulations: increased Ye (similar to jets)
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Panov+ (2014)Mendoza-Temis+ (2014)Shibagaki+ (2015)
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Jets from rotational CCSNe
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Jets from rotational CCSNe
• Have to assume B-field and rotation
• Don’t know initial conditions from stellar evolution
• Cannot computationally follow
Bini � MRI � increasing B � jet ejecta
• But observe NSs with B=1015G
• At low metallicity:
• Less mass loss � loose less angular momentum
• Jets possibly more frequent at low metallicity
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Chemical evolution
NS mergers and/or rotational CCSNe?
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Chemical evolution
• Do NS mergers show up early enough in GCE
to explain all r-process events?
55Argast+ (2004)
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Chemical evolution
• Do NS mergers show up early enough in GCE
to explain all r-process events?
• SN and NS merger rates
56Matteucci+ (2013)
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Chemical evolution
• Do NS mergers show up early enough in GCE
to explain all r-process events?
• SN and NS merger rates
• Mixing in chem evolution models?
• Inhomogeneous chem evolution models
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Inhomogeneous chem evolution
Mixing into 5x106Msun or into 5x104Msun
58Van de Voort+ (2015)See also Shen+ (2015)
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Chemical evolution
Magenta: dataNo magnetorotational jetsGreen/red: different merging time scalesBlue: higher merger rate
Combination of NS mergers and magnetorational jets
59Wehmeyer+ (2015)
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Summary
• Core-collapse SN nucleosynthesis:
• Explosion mechanism matters for nucleosynthesis (and
other questions)
• Induced explosions with PUSH
• Details of neutrino physics and microphysics matter
(neutron-rich versus proton-rich; neutrinp-p-process, (neutron-rich versus proton-rich; neutrinp-p-process,
LEPP)
• R-process:
• Main r-process: always solar proportions, but rare event
• Site: Options include jets from magneto-rotational SNe
and NS mergers, but probably not regular SNe
• Variations of U and Th at low metallicity � indication for
MHD jets (and not robust abundances from NS
mergers)?60