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Strong Magnetic Field (SMaF) in Nuclear Astrophysics Myung-Ki Cheoun Astro Nuclear Physics Group Soongsil University, Seoul, Korea http://ssanp.ssu.ac.kr L. Calçada/ESO Neutrino Physics and Astrophysics, NIST Istanbul, Mar. 16 ~ Mar. 20 , 2015 Collaborators Eunja Ha, Y. S. Kwon, Ki-Seok Choi, T. Miyatsu, M. Kusakabe, Jaewon Shin, Gil-Seok Yang, C-Y. Ryu (Soongsil University) …. Hungchong Kim (Kookmin Univ.), K. S. Kim (Korea Aerospace Univ.) W. So (Kangwon Univ.), C. Hyun (Daegu Univ.)… K. Tsushima (IIP, Brazil), K. Saito (TSU) G. Mathews (Notre Dame), Baha Ballantekin (Wisconsin), Alex Brown (MSU) T. Kajino (NAOJ), Ko Nakamura (Waseda) T. Maruyama (Nihon Univ.), T. Hayakawa (JAEA), S. Chiba (TIT)… C. Deliduman. P. Yamac (Turkey) A. Faessler, F. Simkovic (Tuebingen Univ.)… Contents 0. Introduction 1. Strong Magnetic Field (SMaF) in Dense Matter 1-1. Equation of States in Neutron Stars MKC et.al, PRC 82, 025804, (2010); PRC 83, 018802 (2011); JCAP 10, 21 (2013)… 1-2. Pulsar Kick of Neutron Stars 1-3. Spin Deceleration of Neutron Stars PRD 86 (2012) 123003 ; PRD83 (2011) 081303(R); PRC89 (2014) 035801; PRD 90 (2014) 0637302… 2. Particle Production by SMaF in Astrophysics 2-1. Semi Classical Approach 2-2. Quantum Field Approach 3. Meson Production by SMaF 4. Summary and Conclusions Introduction Neutron Star and SMaF SGR,AXR … , EM and GR waves Courtesy by T. Maruyama Pulsar Kick and Spin Deceleration of Neutron Stars in Supernovae Explosion Introduction Pulsar Kick and Spin deceleration Contents 0. Introduction 1. Strong Magnetic Field (SMaF) in Dense Matter 1-1. Magnetic Field in Neutron Stars MKC et.al, PRC 82, 025804, (2010); PRC 83, 018802 (2011); JCAP 10, 21 (2013)… 1-2. Pulsar Kick of Neutron Stars 1-3. Spin Deceleration of Neutron Stars PRD 86 (2012) 123003 ; PRD83 (2011) 081303(R); PRC89 (2014) 035801; PRD 90 (2014) 0637302… 2. Particle Production by SMaF in Astrophysics 2-1. Semi Classical Approach 2-2. Quantum Field Approach 3. Meson Production by SMaF 4. Summary and Conclusions Formalism Lagrangian with SmaF Formalism Dirac Equation under SmaF Results Magnetic Field Effects in NS MKC et.al, PRC 82, 025804, (2010); PRC 83, 018802 (2011); JCAP 10, 21 (2013)… Eq. of State Results by MTOV and Strong Magnetic fields MKC et.al, JCAP (2013) In np and nph phase with stronger magnetic field -a a For stronger m. field, we obtain more stiffer EOS and more massive Masses !! May compensate modified gravity (alpha >0). Formalism Lagrangian with SmaF + Neutrinos Formalism X-section of Lepton-Baryon Scattering Results Scattering and absorption X-sections Magnetic Field increases neutrin os emitted in the direction parallel to the magnetic field and decreases that in its opposite direction !!! PRD 86 (2012) 123003 ; PRD83 (2011) 081303(R); PRC89 (2014) 035801; PRD 90 (2014) 0637302… Pulsar Kicks Boltzmann Equation Pulsar Kicks Angular Dependence of emitted neutrinos Pulsar Kicks Kick Velocity of Neutron Star Spin Deceleration Toroidal Magnetic Field Spin Deceleration Toroidal Magnetic Field SMaF ⇒ Affect neutrino scattering and absorption in dense matter TM et al., PRD83, 081303(R) (‘11) , PRD86,123003 (‘12), PRC89, 035801 ‘(14) Asymmetry of Neutrino Absorption 4.2 % at ρB=ρ0, 2.2 % at ρB=3ρ0 when T = 20 MeV and B = 1017G Poloidal Magnetic Field Configuration → Kick Velocity vkick ≈ 500 －600 [km/s] when T = 20 MeV and B = 2×1017G Toroidal Magnetic Field Cation → Spin-Down Rate of PNS Spin-Down Ratio P-dot/P ≈ 10-6 ～ 10-7 (1/s) for Asym. ≈ 10-8 (1/s) n –Emit for MDR Perturbation calculation－＞ Non-perturbation including Landau quantization is in progress 24 Contents 0. Introduction 1. Strong Magnetic Field (SMaF) in Dense Matter 1-1. Magnetic Field in Neutron Stars MKC et.al, PRC 82, 025804, (2010); PRC 83, 018802 (2011); JCAP 10, 21 (2013)… 1-2. Pulsar Kick of Neutron Stars 1-3. Spin Deceleration of Neutron Stars PRD 86 (2012) 123003 ; PRD83 (2011) 081303(R); PRC89 (2014) 035801; PRD 90 (2014) 0637302… 2. Particle Production by SMaF in Astrophysics 2-1. Semi Classical Approach 2-2. Quantum Field Approach 3. Meson Production by SMaF 4. Summary and Conclusions SYNCHROTRON RADIATION 1GeV～1TeV of proton ⇒ Synchrotron Radiation ・・・ Pion Production ??? (𝑺𝒕𝒓𝒐𝒏𝒈 𝑭𝒐𝒓𝒄𝒆 > 𝑬. 𝑴𝒂𝒈. 𝑭𝒐𝒓𝒄𝒆) 𝑵𝒆𝒆𝒅 𝒕𝒐 𝒄𝒂𝒍𝒄𝒖𝒍𝒂𝒕𝒆 𝒇𝒓𝒐𝒎 𝒔𝒆𝒎𝒊 − 𝒄𝒍𝒂𝒔𝒔𝒊𝒄𝒂𝒍 𝒕𝒐 𝒒𝒖𝒂𝒏𝒕𝒖𝒎 𝒇𝒊𝒆𝒍𝒅 𝒕𝒉𝒆𝒐𝒓𝒚 Ref: V.L.Ginzburg et al., UsFiN 87, 65, ARA&A 3, 297 (1965) T.Kajino et al., ApJ 782, 70 (2014) However, Scalar particle (not PS particle) PV coupling source term 𝒒⊥𝑩 j qσ Spin Flip process is dominant? Anomalous Magnetic Moment ⇒ Tensor field kinematics §2. Formulation Magnetic Field : Dirac Eq. Wave Function Dirac Spinor Tensor type mean field of ANM Nucleon Green Functional ET P 2 z 2n 1 s M 28 2 N sUT 2 PT2 2n 1 s Decay Width of p to p + p 0 30 πN interaction Pion Momentum Q (0,QT ,Qz ) q eB §3 Results of π0 Production Ei 1 GeV, B 5 1018 G eB 17.2 MeV , nmax e p 2mN B 28.3 MeV si 1 50 for si 1 2 45 for si 1 W/O AＭN nmax si 1 47 2 Decay Width Competition of Spin flip and AMN interaction Ep 300 MeV With AMN --1 → +1 Large Transition momentum |Q| (In particular，Qz) Small Transition Energy ーEπ Without AMN spin flip contribution is much larger !!! TRANSITION STRENGTH IN LANDAU LEVELS ni 45 With AMN Without AMN －1 －> +1 : Energy difference between transition levels becomes small !!! p → p + π0 does not satisfy the energy and momentum conservation in free space, so that it could not happen. In Q.P, we need larger transition energy and smaller 3 momentum transfer for this event. SMaF＋ANM Tensor type Mean field s = +1 （Repulsive）, s = －1 （Attractive） s = －1 → s = +1 Level difference becomes small ⇒ Transition energy becomes large ⇒ Similar to free space kinematics ⇒ Transition rate increases s = +1 → s = － 1 Level difference becomes large ⇒ Transition energy becomes small ⇒ Different to free space kinematics ⇒ Transition rate decreases FUTURE WORKS More Physical Quantities Decay of high energy proton in small B field ～ 1015G n ：Very large (Classical) Laguerre function → Asymptotic form Vector meson ρ, ω, and neutrino production Non-perturbative calculation with Landau quantization which include Temperature, density effects Summary and Conclusion for SMaF Physics 1. We calculated neutrino transport inside PNS, which shows an asymmetry with respect to the magnetic field direction in a magnetar, by exploiting RMF, neutrino scattering and Boltzman equation. 2. The asymmetry turns out to be a source of pulsar kicks of neutron stars. 3. For the spin deceleration of neutron star, we also considered toroidal magnetic field, in which we also found the asymmetry leading to the spin deceleration. 4. Additional source of neutrinos, URCA process is also shown to enlarge the asymmetry. 5. In the Universe, we need more deep understanding of strong magnetic field (SMaF) physics, for example, Landau quantization and polarization of particle propagation inside neutron stars. It may lead to new mechanism of cosmic particles. Thanks for your Attention !! Teşekkur ederim