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Exploring Nucleosynthesis at Strong Magnetization and the Titanium Problem

Investigating the impact of magnetic fields on explosive nucleosynthesis in core-collapse supernovas, focusing on titanium production and decay processes. Analysis of SN1987a, Cassiopeia A, and other supernovas, including observations and theoretical models.

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Exploring Nucleosynthesis at Strong Magnetization and the Titanium Problem

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  1. Nucleosynthesis at strong magnetization and the titanium problem EMIN-2018 V.N.Kondratyev, U.M.Nurtayeva, A.Zh.Zhomartova Physics Department,Taras Shevchenko National University of Kyiv, 03022 UA Kyiv, Ukraine 2 Bogolubov Laboratory of Theoretical Physics, JINR, 141980, Dubna, Russia

  2. Before and after pictures of SN1987a

  3. Hertzsprung- Russell (H-R) diagram Stefan-Boltzmann Law for flux luminosity L of a star with radius R & surface temperature T L~(Surface)T4~R2T4

  4. Stellar Collapse and Supernova Explosion Newborn Neutron Star ~ 50 km Gravitational binding energy Eb 1053,5 erg  20% MSUN c2 This is distributed as 99% Neutrinos 1% Kinetic energy of explosion (1% of this into cosmic rays) 0.01% Photons, outshine host galaxy Neutrino Cooling Proto-Neutron Star nuc 31014 g cm3 T  1 MeV

  5. Core-collapse supernova high-mass(M>8Mo)starEvolution on HR diagram explosive nucleosynthesis origin of Heavy Nuclides

  6. Explosive nucleosynthesis Fe core Mc=1.5Mo

  7. INTEGRALVIRGO.UA Lomonosov, NeuStar

  8. IntegralIBIS/ISGRI

  9. CAS A(3.4+0.3-0.1)kpc, TYCHO(2.2+/-0.3)kpc

  10. Investigated Supernovas Name Coordinate Age SN 1987A - 279.7 -31.9, 31 y Cas A - 111.7 -2.1, 330 y TYCHO - 120.1 +1.4, 440 y Vela Junior - 266.3 -1.2 ?

  11. The scheme of the 44Ti decayEarth environment 59 y

  12. Cassiopeia A (3.4+0.3-0.1)kpc Energy range (keV):20-62-72-82-100

  13. F The direction (i.e.. pixel number) dependence of the registered gamma-ray flux at different energy ranges: 20–62 keV - a, 62–72 keV - b, 72–82 keV – c; for the angle region containing the Cassiopeia A SN remnant. The right bottom panel (d) represents the spectrum from the Cassiopeia A in the energy range 20–95 keV, the solid line shows the fit with the power law energy E dependence, .

  14. Background estimate + Lines K·Ea a=-3.64 +/- 0.09 T= 1.5Ms

  15. SPI detector data Fit results Flux=(5.1+/-1.0) 10-5ph/cm2 s T=1.5 Ms

  16. mass of 44Ti synthesized at Cassiopeia A explosion[VNK et al ‘Nucleus2004’; PhAN (2009)] R–distancetotheobject,T1/2–theelementhalf-life,Na–theAvogadro constant,M–molarmass,I–γ-quantaflux,p-quantumyield,t–remnantage. 5.1 3.3

  17. SN1987 A (50kpc) Energy range (keV):20-62-72-82-100

  18. S.A.Grebenev et al Nature, 490, 373-375 (2012).

  19. THEORY & Observations -1 SN1a Model 10

  20. State Equation (SE): Nuclear Matter VSRegular Liquid(Noble Gas) Van der Waals SE (1875) & Nuclear Matter SE(1983)(relative units: V/Vc; p/pc ; T/Tc ) Instability region H. Jaqaman et al., Phys. Rev. C 27 (1983)2782

  21. D=109 g/cm3 T=0.1 MeV

  22. explosion proceeds through convection processes -sphere magneto-rotationalinstabilities & dynamo-action amplifying Magnetic fields up to strengths hundred tera-tesla

  23. The magnetic field evaluation(S.G.Moiseenko, G.S.Bisnovatyj-Kogan, N.V.Ardeljan, MNRAS 370 (2006) 501)

  24. Magnetic field estimates predominant energy component of shock wave ESoriginates from the magnetic pressure <B2>RR~2ES ~1051,5 ergs R~ 40Km; R~ 1Km B~101 - 102 TeraTesla B(R) ~BR/ R

  25. Magnetic field estimates Magnetic and gravitational forces dB2/dR ~ 8pGM n(R)/R2 4pR2 n(R) = dM/dR B~101.5TeraTesla (M/Mo)(10km/R)2 R~ 40Km; R~ 1Km B~101 - 102 TeraTesla

  26. L or B Magneticfieldsin HIC Magnetic field isinducedthrough the axial anomaly Non-zero angular momentum (or equivalently magnetic field) in heavy-ion collisions B~101.5TeraTesla (E/Eo)1/2

  27. NUCLEAR STATISTICAL EQUILIBRIUM in Ultra-Strong Magnetic Fields Entropy S extremum  Nuclear composition at temperature T Binding Energy B spin-magnetic part in partition function

  28. Nuclear Shell Effects at Ultra-Strong Magnetic FieldsV.N.K. //PRL 2002. V.88, 221101 // J.Nucl.Sci.Technol. V.1 Sup.2. P.550 // J.Nucl.Radiochem.Sci. 2002. V.3. P.205 // PRC 2004 V.69, 038801/ЯФ. 2012 Nucleons Binding Energy Level density With Single particle levels filled up to the Fermi energy

  29. the Hartree self-consistent mean field approach inmagnetic field : h • Single particle Hamiltonian • H = HMF + (so)*(ls) + (Magnetic terms) • Pauli–spin (s) - M (hs) • Landau–orbital (l) - M (hl) :protons

  30. Neutrons Minority spin up Majority spin down

  31. Binding energy of even-even symmetricnucleiat magnetic fields h

  32. Zeeman regime: H< 30 TT Linear response: VNK PLB’18, MNRAS’18

  33. Таб.1 For symmetric nuclei

  34. relative yield y=Y(H)/Y(0) [i/56Ni]:44Ti -1; 48Cr -2; 60Zn -3; Магнитное поле, h

  35. SUMMARY • We analyze the synthesis and decay of n nuclides in SNRs • Obtained the spectra and flux for the specific lines of decay products

  36. SUMMARY • Magnetism of Atomic Nuclei Thermodynamic formalism • Magnetic field effect on Nuclear Structure at • Pauli type Paramagnetic Response • Landau-type Orbital Magnetism • Magnetic fields of Tera-Tesla encrease of Binding Energy of Nuclei of Smaller Masses approaching Ti-44 • Enhancement in Yield at nucleosynthesis

  37. relative yield y=Y(H)/Y(0)56Ni(solid) і 44Ti(dashed line) Магнитное поле, h

  38. Averaging over MRI Volume a = DB(H0) kT b=(ra/r0)2 интегральная показательная функция

  39. Galactic chemical evolution

  40. SUMMARY • We analyze the synthesis and decay of n nuclides in SNRs • Obtained the spectra and flux for the specific lines of decay products

  41. SUMMARY • Magnetism of Atomic Nuclei Thermodynamic formalism • Magnetic field effect on Nuclear Shell Structure Phase-shift in shell oscillations of Nuclear Masses • Pauli type Paramagnetic Response • Landau-type Orbital Magnetism • Magnetic fields of Tera-Tesla shiftNuclear Magics of Iron region towards Smaller Masses approaching Ti-44 • Enhancement in Yield at nucleosynthesis

  42. SUMMARY • We analyze the synthesis and decay of 44Ti in SNRs • Obtained the spectra and flux for the lines of 44Sc

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