Exploring Hadron Physics in Black Hole Formation: a New ... · Exploring Hadron Physics in Black...
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Exploring Hadron Physics in Black Hole Formation: a New Promising Target of Neutrino Astronomy
Ken’ichiro Nakazato(Department of Astronomy, Kyoto University)
in collaboration with K. Sumiyoshi(Numazu CT),H. Suzuki(Tokyo U of Sci.)
and S. Yamada(Waseda U)
New Frontiers in QCD 2010 @ YITP, Kyoto U, January 29, 2010
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Outline1. Introduction
Equation of state (EOS)
of hot and dense matter and stellar core collapse
2. Core collapse simulationImpact of EOS and neutrino signal
3. Neutrino detectionStatistical analyses
4. Conclusion
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1. Introduction
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Fates of massive stars
Normal SN
Nomoto+ (2006)
• Stars with > 10Msolar make a gravitational col- lapse and, possibly, a supernova explosion.
• Stars with > 25Msolar are thought to form a black hole (BH).
• Observations show2 branches.– Hypernovae(Rapid rotation)
– Faint or FailedSupernovae
(Weak rotation)
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Failed supernova neutrinos• Failed supernova progenitor makes bounce
once and recollapse to the black hole.• In this process, temperature and density of
central region gets a few times 10 MeV and a few times ρ0 (saturation density of nuclear matter), and a lot of neutrinos are emitted.
Bounce
Black holeν
ν
ν
Proto-neutron star
Mass accretionCore Collapse
Massive starν
ν
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Motivation• Can we probe into physics of hot and dense
matter (including hyperons and quarks) by the black hole formation?
→ observable: Neutrinos!T
ρ0
Quark Phase~150MeV Mixed Phase
Hadronic Phase
Black Hole Formation
accelerator
Ear
ly
Uni
vers
e
Compact starsStellar Collapse
ρ0
Hyperons
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Aims of this study• Thus, property of hot and dense matter is
also a target of neutrino astronomy.– Equation of State (EOS)
of nuclear matter
– Hyperon (Ishizuka+ 2008, Sumiyoshi+ 2009)
– QCD transition (Nakazato+ 2008a, in prep.)
• Evaluate the ν
event number from failed supernovae with 40Msolar non-rotating progenitor.
• Investigate the EOS dependences of ν signal.
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Nakazato et al. (2008b)
νe⎯νe
νx
• Numerical simulations of black hole formation
• Spectra of emitted neutrinos
• Event numbers on the detector(SuperKamiokande) → Discussion
Brief sketch of our study
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Nakazato et al. (2008b)
νe⎯νe
νx
• Numerical simulations of black hole formation
• Spectra of emitted neutrinos
• Event numbers on the detector(SuperKamiokande) → Discussion
Brief sketch of our study
Neutrino Oscillation
Neutrino reactionin the detector
Detectability(e.g. energy resolution)
Progenitor model
EOS of hot dense matter
General relativistic hydrodynamics
Neutrino reactions and transports
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2. Core collapse simulation
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Hydrodynamics & Neutrinos
Spherical, Fully GR Hydrodynamics metric:Misner-Sharp (1964)
mesh:255 non uniform zones
+Neutrino Transport (Boltzmann eq.)Species : νe ,⎯νe ,
νμ
(
= ντ ) ,⎯νμ (
=⎯ντ )
Energy mesh : 14 zones (0.9 – 350 MeV)Reactions : e- + p ↔
n + νe , e+ + n ↔
p +⎯νe , ν + N ↔
ν + N,
ν + e ↔
ν + e, νe + A ↔
A’ + e-, ν + A ↔
ν + A,e- + e+ ↔
ν +⎯ν, γ* ↔
ν +⎯ν, N + N’ ↔
N + N’ + ν +⎯ν
Yamada, Astrophys. J. 475 (1997), 720Yamada et al., Astron. Astrophys. 344 (1999), 533
Sumiyoshi et al., Astrophys. J. 629 (2005), 922
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List of equations of state• Current status
– Lattimer-Swesty (LS) EOS,• Liquid drop model with Skyrme interactions (1991)• 3 choices of incompressibility: K = 180, 220, 375 MeV
– Shen EOS• Relativistic Mean Field theory (Shen et al. 1998)
– Hyperon + pion EOS• Shen-EOS with hyperons (Ishizuka et al. 2008)
– Quark + pion EOS• Shen-EOS with MIT Bag model (Nakazato et al. 2008a)
• Future work– Quark + hyperon + pion EOS
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List of equations of state• Current status
– Lattimer-Swesty (LS) EOS,• Liquid drop model with Skyrme interactions (1991)• 3 choices of incompressibility: K = 180, 220, 375 MeV
– Shen EOS• Relativistic Mean Field theory (Shen et al. 1998)
– Hyperon + pion EOS• Shen-EOS with hyperons (Ishizuka et al. 2008)
– Quark + pion EOS• Shen-EOS with MIT Bag model (Nakazato et al. 2008a)
• Future work– Quark + hyperon + pion EOS
Already utilized in our numerical simulations.
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Results for “nucleonic” EOS’s
• Shen EOS is hardest (K = 281 MeV).• Harder EOS has longer ν
emission.
• Softer EOS has high ν
luminosity.
LS180566 ms
LS220784 ms
Shen1345 ms
time after bounce (s)
tota
l lum
inos
ity (
erg/
s)
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Role of matter property • Determining hardness of Equation of State (EOS).– Soft EOS is easy to compress.– Maximum mass of compact
star is lower for soft EOS.
• Inside the failed supernovae…– For soft EOS, more compressed,
T ↗, ν
energy and luminosity ↗.– For soft EOS, BH formation is
fasten due to low maximum mass.
psoft EOS
hard EOS
ρ
ν
ν
Mass accretion (ram pressure)
Proto-neutron star
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Hyperon EOS
• Relativistic Mean Field Theory– extension of Shen EOS to the baryon octet
• Latest experimentalresults for potentialsare taken into account.– UΛ
= -30 MeV– UΣ
= 30 MeV (repulsive)
– UΞ
= -15 MeV
• Data with thermal pionsis also prepared.
Ishizuka et al., J. Phys. G 35, (2008), 085201
0
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Collapse with hyperon EOS
time after bounce (s)0.0 0.5
1
10
100
103
104
radi
us (
km)
np
α
Λ
radius (km)0 10 20
fract
ion
1
0.1
0.01
10-3
10-4
Sumiyoshi et al., Astrophys. J. Lett. 690 (2009), 43
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Collapse with hyperon EOS
time after bounce (s)0.0 0.5
1
10
100
103
104
radi
us (
km)
np
α
Λ
radius (km)0 10 20
fract
ion
1
0.1
0.01
10-3
10-4
radius (km)0 10 20
fract
ion
1
0.1
0.01
10-3
10-4
n
p
ΛΣ−
Ξ−
α
Sumiyoshi et al., Astrophys. J. Lett. 690 (2009), 43
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Collapse with hyperon EOS
• Hyperons appear for the late phase.
time after bounce (s)0.0 0.5
1
10
100
103
104
radi
us (
km)
np
α
Λ
radius (km)0 10 20
fract
ion
1
0.1
0.01
10-3
10-4
radius (km)0 10 20
fract
ion
1
0.1
0.01
10-3
10-4
n
p
ΛΣ−
Ξ−
α
radius (km)0 10 20
fract
ion
1
0.1
0.01
10-3
10-4
n
pΛ
Ξ−
Σ−
Ξ0
Σ0
α
Sumiyoshi et al., Astrophys. J. Lett. 690 (2009), 43
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Hadron-quark mixed EOS
• Shen EOS with pions for Hadronic phase
• MIT Bag model (Chodos et al. 1974)
for Quark phase– Bag constant: B = 250 MeV/fm3
• Gibbs conditions are satisfied in Mixed phase.– μn = μu + 2μd , μp = 2μu + μd
– PH = PQ
β equilibrium (ν trapping) is assumed in Mixedand Quark phase.– μd = μs , μp + μe = μn + μν
Nakazato et al., PRD 77 (2008a), 103006
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Collapse with quark EOS
• Quark transition occurs at the very late phase and trigger the black hole formation.
Nakazato et al., arXiv:1001.5084
radius (km)0 10 20
fract
ion
1
0.5
0
1015
1013
n
pπ
27 ms before BH formation
dens
ity (
g/cm
3 )
radius (km)0 10 20
1
0.5
0
1015
1013
radius (km)0 10 20
0.07 ms before BH formation at BH formation
n
pd
u
s
n
p
d us
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Results for “exotic” EOS’s
• Hyperons and quarks (with pions)
shorten the duration of ν
emission.
• But, not affect the ν
luminosity very much.
hyperon682 ms
quark + π1049 ms
Shen1345 ms
time after bounce (s)
tota
l lum
inos
ity (
erg/
s)
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Short summary • For nucleonic model, soft EOS has short
duration and high luminosity ν
emission.• Hyperons and quarks shorten the duration
but not affect ν
luminosity very much.
• However, there is a question.
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Short summary
• Can we distinguish hyperonic model from soft nucleonic models?
LS180566 ms
LS220784 ms
hyperon682 ms
time after bounce (s)
tota
l lum
inos
ity (
erg/
s)
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3. Neutrino detection
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Oscillation of failed supernova ν• Neutrino oscillation occurs before detection.• But there are undetermined parameters,
namely sin2θ13 < 0.02 and mass hierarchy.→ Neutrino oscillation and its parameter
dependence should be evaluated.Neutrino sphere
oscillation by MSW effect
Stellar envelope vacuum oscillation
Nakazato et al., PRD 78 (2008b), 083014
R
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Neutrino event number• Neutrino flux is scaled as ∝ 1 / R2
• Event number is comparable to that of ordi- nary SN ν (~ 10000 for events in our Galaxy).
• Event number depends also on the mixing parameters.
EOS Normal & sin2θ13 =10−8
Inverted & sin2θ13 =10−2
Hyperon 16,490 9,952LS180 16,086 12,136LS220 25,978 23,656
Event numbers for R = 10 kpc, but R may be undetermined
from obs…
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Statistical analyses• Normalize cumulative event numbers by total
event number till 0.5s after bounce, N0.5s , and assume N0.5s = 10000 (event in our Galaxy).
• Perform Monte Carlo simulation for detection based on numerical data of Hyperon case, and compare it to numerical data of LS cases.
• Judge these cases are distinguished or not by Kolmogorov-Smirnov test.
• Merit of this method;– We do not have to take care of the distance to
the source and ν
emission after BH formation.
Nakazato et al., submitted to PRL.
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Result of the fitting (N0.5s = 10000)
• They are distinguishable with 99% C.L. for both mixing parameter sets.
LS220LS180
(Numerical)
Hyperon(Monte Carlo)
10000
8000
0
6000
4000
2000
0 0.1 0.2 0.3 0.4 0.5
10000
8000
0
6000
4000
2000
cum
ulat
ive
even
t num
ber
time (s)0 0.1 0.2 0.3 0.4 0.5
time (s)
Normal & sin2θ13=10-8 Inverted & sin2θ13=10-2
LS220LS180
(Numerical)
Hyperon(Monte Carlo)
cum
ulat
ive
even
t num
ber
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Result of the fitting (N0.5s = 400)
• The distinction is difficult for left case but fea- sible for right case (90% of MC simulations).
LS220LS180
(Numerical)
Hyperon(Monte Carlo)
400
300
0
200
100
0 0.1 0.2 0.3 0.4 0.50
cum
ulat
ive
even
t num
ber
time (s)0 0.1 0.2 0.3 0.4 0.5
time (s)
Normal & sin2θ13=10-8 Inverted & sin2θ13=10-2
LS220LS180
(Numerical)
Hyperon(Monte Carlo)
cum
ulat
ive
even
t num
ber 400
300
200
100
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4. Conclusion
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Summary• We have performed a series of black-hole-
forming core collapse simulations for non- rotating 40Msolar star with various EOS’s.
• We have found that EOS affects the emission duration and luminosity of ν.
• Differences in ν
light curve is statistically distinguishable by SuperKamiokande for the progenitors in our Galaxy.
→ These results implies possibilities to probe the properties of hot and dense nuclear matter from neutrino astronomy.
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Future work• More EOS’s.
– EOS with quarks, hyperons and pions.– EOS by other frameworks (e.g., many body
theory etc.)
• More initial models.– Mass loss and convection may affect the density
profile of outer layer.
• Multi dimensional Effect– Rotation– Magnetic field
→ This is the beginning!!