Neutrino phenomenology Lecture 3: Aspects of neutrino astrophysics
Aspects of the Astrophysics and Nuclear Physics of r -Process Nucleosynthesis
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Transcript of Aspects of the Astrophysics and Nuclear Physics of r -Process Nucleosynthesis
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Aspects of the Astrophysics and Nuclear Physics
of r-Process Nucleosynthesis
Rebecca SurmanUnion College
Workshop on Statistical Nuclear Physics and Applications in Astrophysics and Technology
July 2008
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r-process nucleosynthesis
R Surman, Astrophysics and Nuclear Physics of the r process, SNP 08 2/25
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r-process nucleosynthesis - current challenges
Astrophysics
The astrophysical site(s) not conclusively known; possibilities include:
• core collapse supernovae e.g., Meyer et al (1992), Woosley et al (1994), Takahashi et al (1994)
• neutron star mergers e.g., Meyer (1989), Frieburghaus et al (1999), Rosswog et al (2001)
• shocked surface layers of O-Ne-Mg cores e.g., Wanajo et al (2003), Ning et al (2007)
• gamma-ray bursts e.g., Surman et al (2005)
Nuclear Physics
Nuclear properties for ~3000 nuclei far from stability
nuclear masses fission probabilities, distribution of fragments
beta decay rates neutron capture rates (?)
R Surman, Astrophysics and Nuclear Physics of the r process, SNP 08 3/25
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halo star observations
Cowan et al (2006)
R Surman, Astrophysics and Nuclear Physics of the r process, SNP 08 4/25
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halo star observations
Main r process
Cowan et al (2006)
R Surman, Astrophysics and Nuclear Physics of the r process, SNP 08 5/25
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halo star observations
Weak r process Main
r process
Cowan et al (2006)
core collapse supernovae ?
R Surman, Astrophysics and Nuclear Physics of the r process, SNP 08 6/25
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the SN neutrino-driven wind
Important parameters
outflow timescale
entropy
electron fraction€
ρ ~ e−t / 3τ ; τ ~ 0.01 s to τ ~ 1 s
€
s ~ 100 to s ~ 400
€
Ye =1
1+ n / p; Ye ~ 0.3 to Ye ~ 0.5
p, n 4He + n seed nuclei + n r process
PNS
shock
€
p + ν e ↔ n + e+
n + ν e ↔ p + e−
€
Tv e> Tve
R Surman, Astrophysics and Nuclear Physics of the r process, SNP 08 7/25
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the main r process
How is a consistent pattern achieved?
Ye = 0.27
Ye = 0.26
Ye = 0.25
R Surman, Astrophysics and Nuclear Physics of the r process, SNP 08 8/25
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low Ye main r process
QuickTime™ and aTIFF (Uncompressed) decompressor
are needed to see this picture.
Beun, McLaughlin, Surman, & Hix, PRC 77, 035804 (2008)
R Surman, Astrophysics and Nuclear Physics of the r process, SNP 08 9/25
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low Ye main r process
QuickTime™ and aTIFF (Uncompressed) decompressor
are needed to see this picture. Fission Cycling
Beun, McLaughlin, Surman, & Hix, PRC 77, 035804 (2008)
R Surman, Astrophysics and Nuclear Physics of the r process, SNP 08 9/25
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fission cycling and the neutrino luminosities
Surman, Beun, McLaughlin, Kane, & Hix, J Phys G 35, 014059 (2008)
(1051 erg/s)
(1
051 e
rg/s
)
€
p + ν e ↔ n + e+
n + ν e ↔ p + e−
R Surman, Astrophysics and Nuclear Physics of the r process, SNP 08 10/25
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fission cycling: comparison with halo star data
Beun, McLaughlin, Surman, & Hix, PRC 77, 035804 (2008)
QuickTime™ and aTIFF (Uncompressed) decompressor
are needed to see this picture.
R Surman, Astrophysics and Nuclear Physics of the r process, SNP 08 11/25
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fission cycling and the main r process
In the SN neutrino-driven wind, the electron neutrino flux determines whether a successful r process is possible
The electron neutrino flux can be reduced by:
fast outflow
active-sterile neutrino oscillations
other new physics
If a sufficient reduction in the electron neutrino flux occurs, fission cycling may insure a stable abundance distribution consistent with the pattern in metal-poor halo stars
Accurate fission probabilities and fragment distributions are required to correctly predict the details of the final abundance distribution for a fission cycling main r process.
R Surman, Astrophysics and Nuclear Physics of the r process, SNP 08 12/25
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black hole - neutron star merger
Orbit of a black hole - neutron star binary decays by gravitational wave emission
Tidal disruption of the neutron star produces a rapidly accreting disk around the black hole (AD-BH)
possible engine for a short gamma-ray burst
QuickTime™ and aYUV420 codec decompressor
are needed to see this picture.
animation credit: NASA/SkyWorks Digital
R Surman, Astrophysics and Nuclear Physics of the r process, SNP 08 13/25
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PNS – AD-BH comparison
accretion disk
PNS BH
jet (?)
shock
outflow
R Surman, Astrophysics and Nuclear Physics of the r process, SNP 08 14/25
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PNS – AD-BH nuclear physics
accretion disk
PNS BH
jet
shock
outflow
neutrino scattering and emission
nucleosynthesis
nucleosynthesis jet (?)
nuclear physics of disk
nuclear physics of core
R Surman, Astrophysics and Nuclear Physics of the r process, SNP 08 15/25
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3D black hole - neutron star merger model
1.6 M neutron star + 2.5 M black hole with a = 0.6
Evolved until remains of neutron star form an accretion disk
Model by M. Ruffert and H.-Th. Janka
R Surman, Astrophysics and Nuclear Physics of the r process, SNP 08 16/25
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neutrino temperatures
Surman, McLaughlin, Ruffert, Janka, and Hix, arXiv:0803.1785
€
Tv e> Tve
nv e> nve
R Surman, Astrophysics and Nuclear Physics of the r process, SNP 08 17/25
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Adiabatic flow with velocity as a function of radial distance:
with v ~ 104 km/s, 0.2 < < 1.4, 10 < s/k < 50€
u = v∞ 1−Ro
R
⎛
⎝ ⎜
⎞
⎠ ⎟β
our nucleosynthesis calculation
Outflow parameterization
Surman, McLaughlin, Ruffert, Janka, and Hix, arXiv:0803.1785
R Surman, Astrophysics and Nuclear Physics of the r process, SNP 08 18/25
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sample nucleosynthetic outcomes
Surman, McLaughlin, Ruffert, Janka, and Hix, arXiv:0803.1785
All trajectories from the inner disk region make r-process nuclei
This is a direct consequence of the neutrino physics
R Surman, Astrophysics and Nuclear Physics of the r process, SNP 08 19/25
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sample nucleosynthetic outcomes
Möller et al (2003)
Möller et al (1997)
Möller et al (2003) + exp
R Surman, Astrophysics and Nuclear Physics of the r process, SNP 08 20/25
Example: the importance of beta decay rates
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neutron capture rates and the r process
Do they make any difference?
can influence time until onset of freezeout e.g., Goriely (1997,8), Farouqi et al, Rauscher (2005)
can shape local details of the abundance distribution e.g., Surman et al (1998), Surman & Engel (2001)
R Surman, Astrophysics and Nuclear Physics of the r process, SNP 08 21/25
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mass model - neutron capture rate comparison
Surman, Beun, McLaughlin, and Hix, arXiv:0806.3753
Neutron capture rate variation
Mass model variation
R Surman, Astrophysics and Nuclear Physics of the r process, SNP 08 22/25
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nonequilibrium effects of individual capture rates
130 peakrare earth region + 195 peak€
λγ ∝T 3 / 2 exp −Sn
kT
⎛
⎝ ⎜
⎞
⎠ ⎟ σv
Z ,A
€
σv 131 Cd×10
€
σv 131 Sn×100
Surman, Beun, McLaughlin, and Hix, arXiv:0806.3753
R Surman, Astrophysics and Nuclear Physics of the r process, SNP 08 23/25
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influential neutron capture rates
Capture rates that affect a 5-40% change in the global r-process abundance pattern for increases to the rate by a factor of:
10 50 100-1000
Surman, Beun, McLaughlin, and Hix, arXiv:0806.3753
R Surman, Astrophysics and Nuclear Physics of the r process, SNP 08 24/25
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summary
We still don’t know where the r process takes place
evidence increasingly points to core collapse supernovae for the site of the main r process (fission cycling would help)
list of potential sites should include hot outflows from black hole-neutron star mergers, particularly for the weak r process
Everybody knows we need nuclear masses and beta decay rates
individual neutron capture rates are also important
fission probabilities and fragment distributions may be crucial
R Surman, Astrophysics and Nuclear Physics of the r process, SNP 08 25/25