Chiral symmetry breaking in strong magnetic fields
Abstract
Ultra strong magnetic field could be there in the interior of neutron stars.Strong magnetic field can also be produced inheavy ion collision experiments. I will discuss chiral symmetry breaking inhot and dense quark matter in presenceof strong magnetic field within a 3 flavor Nambu Jona Lasinio model. Whilemagnetic catalysis of chiral symmetrybreaking is expected for hot matter, inverse magnetic catalysis for chiralsymmetry breaking is expectedat finite chemical potential. The equation of state for strange quark matteris derived within the model. The effect of pressureanisotropy of dense quark matter in presence of magnetic field in the grossstructural properties of neutron stars will also be discussed.
26/12/2011 at 4:00 pm
Prof. X. Vinas, University of Barcelona
General Seminar
Lecture Hall Block A, Institute of Physics
Document Date:
SEMICLASSICAL APPROXINATION TO PAIRING IN THE WEAK COUPLING REGIME: NUCLEI, COLD ATOMS AND NEUTRON STARS
SEMICLASSICAL APPROXINATION TO PAIRING IN THE WEAK COUPLING REGIME: NUCLEI, COLD ATOMS AND NEUTRON STARS
Abstract
Two issues are treated in this talk: (i) the generic fact that if a fermionic superfluid in the BCS regime overflows from a narrow container into a much wider one, pairing is much suppressed at the overflow point. Physical examples in cold atoms, neutron stars and nuclei where this feature may play an important role are discussed. (ii) A Thomas-Fermi (TF)approach to inhomogeneous superfluid Fermi-systems is presented and shown that it works well in cases where the Local Density Approximation (LDA) breaks down.
Within the framework of the nucleon-meson exchange picture known as therelativistic mean field (RMF) model, we study the bulk properties ofnuclei at different regions of the nuclear chart. Mostly the structure ofsuperheavy elements and the sub-structure of intermediate mass nuclei willbe discussed. We will also derive the NN interaction from the RMFlagrangian which will be apply to study the cluster radioactivity andproton emission phenomenon.References:[1] S. K. Patra, M. Bhuyan, M. S. Mehta, Raj K. Gupta Phys. Rev. C 80034312 (2009).[2] M. Bhuyan et al. Phys. Rev. C 82, 064602 (2010).[3] M. Bhuyan et al. Phys. Rev. C 84, 014317 (2011).[4] M. Bhuyan et al. Int. J. Mod. Phys. E 20 2217 (2010).[5] B. K. Sahu, M. Bhuyan, S. Mohapatro, S. K. Patra. Int. J. Mod. Phys. E 20 2227 (2011).[6] B. B. Singh, M. Bhuyan, Raj. K. Gupta, S. K. Patra, J. Phys. G 34(press) 2012.[7] M. Bhuyan et al. Phys. Lett. B (communicated)
