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• IntroductionIntroduction• Rapid nucleosynthesis – models and sitesRapid nucleosynthesis – models and sites• R-process under high neutron environmentR-process under high neutron environment• Fission in the r-process Fission in the r-process • (n,f)- and (n,f)- and -delayed fission-delayed fission• fission cyclingfission cycling• sf sf – predictions – predictions • Theoretical Abundance of heavy nuclei Theoretical Abundance of heavy nuclei • Superheavy nuclei and cosmochronometersSuperheavy nuclei and cosmochronometers• ConclusionConclusion
Models for spontaneous fission of heavy nuclei and Models for spontaneous fission of heavy nuclei and nucleosynthesis of cosmo-chronometers in the r-process.nucleosynthesis of cosmo-chronometers in the r-process.
Panov IgorPanov Igor((ITEPITEP, , NGU NGU))
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s-, r- processes
SHE
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nucleosynthesis beyond Fe-peak – nucleosynthesis beyond Fe-peak – r-r-process andprocess and s-processs-process
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4
r-process andr-process and s-process pathss-process paths
supernovae
NSMNSM
J.TruranJ.Truran
windswinds
Nuclear data for the r-process: ~6000 nuclei are involved900 nuclei hasT12 > 1 hour
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нуклеосинтез в реакциях с нейтронами (нуклеосинтез в реакциях с нейтронами (s-s-процесспроцесс))::
105106 107 129
Pd Ag Cd n << nn<1012
Z=46
Z=47
Z=48
108 109 110
109 110
110 111 112109
108107
108108
111
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нуклеосинтез в реакциях с нейтронами (нуклеосинтез в реакциях с нейтронами (r-r-process)process)::
126127 128 129
Ag Cd In n (s-процесс: n << nn>1022 nn<1012
Z=47
Z=48
Z=49
130
Waiting point
129 130 131
130 131
131 132 133
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SnII SnII ,, ~ ~ 0 exp(-t/exp(-t/hyd),), hyd < < 10ms10ms
Merging of close binaries:Merging of close binaries: NSNS, NSBHNSNS, NSBH
high n/seeds > 150, Thigh n/seeds > 150, T99< 1, Y< 1, Yee < 0.1 < 0.1
Neutrino-inducedNeutrino-induced rr--process process 44He(He(,,’ n)’ n)33HeHe
Explosions on the NS surfaceExplosions on the NS surface
Hot Hot -wind, high entropy wind -wind, high entropy wind
– – thermonuclear Sne, jetsthermonuclear Sne, jets ? ?
Other objects and processes?Other objects and processes?
2. Main conditions for the r2. Main conditions for the r--processprocess:: ((seedsseeds); ); free neutrons; n/seeds; freezout free neutrons; n/seeds; freezout
Wasserburg, G., Busso, M., & Gallino, R. 1996, ApJ, L109
2 2 objects /scenario: Main r-process - Weak r-objects /scenario: Main r-process - Weak r-process process
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weak r-process SNIa- Truran & Cowan He-flash 1983- Blinnikov, Panov, Ptytsin, Chechetkin 1995
SNIIneutrino-induced r-process-Nadyozhin, Panov, Blinnikov A&A, 335, 1998
NSM-model, main r-process?Freiburghaus et al., AJL 525, 1999 NS+BHJanka, Wanajo, 20011
Blinnikov, S. I., et al. Pazh, 10, (1984) 422Lattimer et al., AJ 213, 225 (1977)
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fission
3. R-process under high neutron density environment – in NSM
Observed Nr
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fissionfission
decaydecay
PPkn (k=0,1,2,3)
Network calculations of the r-processNetwork calculations of the r-process
(n,) (n)
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Nuclear data for the r-process (up to 6000 nuclei )
• beta-decay,
•Cross-sections and reaction rates (n,g), (n,f), ..
• beta-delayed processes Pin, Pdf
• spontaneous fission, sf
•Mass distribution of fission products•Alpha-decay, •Nuclear masses and fission barriersData base of common usage
JINA - Joint Institute of Nuclear AstrophysicsJINA - Joint Institute of Nuclear Astrophysics
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• Seeger, Fowler, et al. (1965) ; Ohnishi (1977) • Thielemann, Metzinger, Klapdor, Zt.Phys., A309 (1983) 301. Pdf=100%• Goriely et al. Astron. Astrophys. 346, 798–804 (1999) s.f. (Swiatecky)• Panov et al., Nucl. Phys. A, 718 (2003) 647. (n,fission) vs Pdf
• I.Korneev et al. NIC-2006; Astronomy Letters, 66 (2008) 131 Yff(Z,A)• Kelic, et al., Phys. Lett. B. 616 (2005) 48 Yff(Z,A)• I.V. Panov, E. Kolbe, F.-K. Thielemann, T. Rauscher, B. Pfeiffer, K.-L. Kratz.
NP A 747 (2005) 633 (n,fission) (n,) Pdf
• G.Martinec-Pinedo et al, Progress in Particle and Nuclear Physics, 59 (2007) 199. (n,fission) vs Pdf
• Y.-Z. Qian, Astron. J. 569 (2002), p. L103. induced fission
• Kolbe, Langanke, Fuller. Phys Rev Lett. 2004 induced fission • I. Petermann et. al. NIC-2008; G.Martinec-Pinedo et al, Progr. in Particle
and Nucl. Phys., 59 (2007) 199-205: (n,fission), Pdf , s.f., induced f..• Panov et al. AA 2010Panov et al. AA 2010 (n,fission) and (n,) • Petermann Martinec-Pinedo Langanke Panov Thielemann SHE AA2012• Panov, I.Korneev, Yu. Lutostansky, F.-K. Thielemann. Yad.Fiz. 2013. Pdi
4. fission in the r-process and rates fission in the r-process and rates calculationscalculations
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nf , nf , nn andand rates rates comparison comparison
for U (left) and Cm (right)for U (left) and Cm (right)nn, nf, , nf, n – Hauser-Feshbach predictionsn – Hauser-Feshbach predictions
, , dfdf, - QRPA, - QRPA
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6. Fission cycling during r-process for NSM conditions 6. Fission cycling during r-process for NSM conditions (t-duration time of the r-process; t=0 - initial composition)(t-duration time of the r-process; t=0 - initial composition)
Neutron star mergers modelling: Rosswog et al. 1999R-process: Panov I., Thielemann F.-K. AL, 30 (2004) 711
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6. Fission cycling – fission fragments are involved in the r-process as new seeds
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I.Petermann, A.Arcones, A.Keli´c, K.Langanke, G.Martínez-Pinedo, W.Schmidt, K-H.Hix, I. Panov, T. Rauscher, F.-K. Thielemann, N.Zinner, NIC-2008;
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R=∫i(t) / ∑i ∫ i(t)dt
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: Bf < Sn; : nuclei with Bf ≥ Sn; inclined crosses: nuclei with neutron binding energy predicted by the ETFSI Sn ~ 2 MeV; and dots: nuclei in which 2 > Sn > 0. 20
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7. Spontaneous fission 7. Spontaneous fission ratesrates
• LgLg((sf sf )) ~ B~ Bff (Frankel&Metropolis,1947) : (Frankel&Metropolis,1947) :
LgLg((sf sf ) =) = 33,3-7,77B33,3-7,77Bff(exp) (exp) (1) (1)
LgLg((sf sf )) =50,127-10,145B=50,127-10,145Bff(etfsi) (etfsi) (2) (2)
• LgLg((sf sf ) = ) = --11461146,,4 + 754 + 75,,33ZZ22//A A –– 11,,638(638(ZZ22//AA))22
+ 0+ 0,,012(012(ZZ22//AA))33 --(7(7,,24 24 --00,,095095ZZ22//AA))BBf f (3)(3)
Zagrebaev, Karpov 2012 (Zagrebaev, Karpov 2012 (Swiatecki, 1957)Swiatecki, 1957)
• Macro-micro model, Smolanchuk et al. Macro-micro model, Smolanchuk et al. 19971997 (4) (4)
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Bf ETFSI- Mamdouh et al., NP 2001
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R-process path and abundances YA(Z,N) when duration r ~ 10s
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nn < 1022 cm-3, n < Squares – most abundant nucleiWhite dots: 10% < Pdf < 90%
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25
nn < 1012, n <<
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JINR => Zagrebaev et al. Phys. Rev. C 84, 044617 (2011)
Amax(progenitors) ≈280
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A(progenitors) ~ < 260
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Final abundances YFinal abundances YA , R ~ 0.4 – 4 109 years
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Final abundance YA when s.f. rates ~
f(Bf)
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Final YA when s.f.rates - macro-micro model
30
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ConclusionsConclusions• It was shown that s.f. model applied to the r-It was shown that s.f. model applied to the r-
process nucleosynthesis strongly influe in first process nucleosynthesis strongly influe in first turn on yields of nuclei-cosmochronometersturn on yields of nuclei-cosmochronometers
• Among tested models of spontaneous fission Among tested models of spontaneous fission phenomenological model based on Swiatecki phenomenological model based on Swiatecki model and on macro-micro model predictions model and on macro-micro model predictions gave the better results in calculation of yields gave the better results in calculation of yields of nuclei–cosmochronometersof nuclei–cosmochronometers
• Additionally to 232/235, 235/238 pairs of Additionally to 232/235, 235/238 pairs of nuclei-cosmochronometers, pairs 232/244 or nuclei-cosmochronometers, pairs 232/244 or 238/244 can be considered238/244 can be considered
• The detailed investigation of decay chain is The detailed investigation of decay chain is neededneeded
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Thank youThank you !!
• Participants for attentionParticipants for attention
• Blinnikov, Dolgov, Korneev, Blinnikov, Dolgov, Korneev, Thielemann Thielemann for for collaborationcollaboration
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Fission cycling – fission fragments are involved in the r-process as new seeds
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Bf TF Myers, Swiatecky 1999
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Map of nuclei and field of Map of nuclei and field of ratesrates
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o - “солнечная” распространенность элементов синим цветом – расчет для сценария слияния нейтронных звезд в двойной системе ( Панов, Корнеев и Тилеманн. Письма в АЖ, т.34, 2008;)
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ModelModel, , SSSS and and metal-poor halo star CS 22892-052
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