Myung-Ki Cheoun

Equation of state for neutron stars in SU(3) flavor symmetry

Using several relativistic mean field models (such as GM1, GM3, NL3, TM1, FSUGold and IU-FSU) as well as the quark-meson coupling model, we calculate the particle fractions, the equation of state, the maximum mass and radius of a neutron star within relativistic Hartree approximation. In determining the couplings of the isoscalar, vector mesons to the octet baryons, we examine the extension of SU(6) spin-flavor symmetry to SU(3) flavor symmetry. Furthermore, we consider the strange (

Neutron stars in a perturbative f(R) gravity model with strong magnetic fields

\sigma^{\ast}

SUPERNOVA NEUTRINO NUCLEOSYNTHESIS OF THE RADIOACTIVE 92Nb OBSERVED IN PRIMITIVE METEORITES

and

Neutrino–nucleus reactions via neutral and charged currents by the quasi-particle random phase approximation (QRPA)

\phi

Coulomb sum rule in the quasielastic region

) mesons, and study how they affect the equation of state. We find that the equation of state in SU(3) symmetry can sustain a neutron star with mass of

Medium effects of magnetic moments of baryons on neutron stars under strong magnetic fields

(1.8 \sim 2.1) M_{\odot}

Ambiguities of neutrino (antineutrino) scattering on the nucleon due to the uncertainties of relevant strangeness form factors

even if hyperons exist inside the core. In addition, the strange vector (

Asymmetric neutrino emission from magnetized proto-neutron star matter including hyperons in relativistic mean field theory

\phi

Cosmological solutions to the Lithium problem: Big-bang nucleosynthesis with photon cooling,

) meson and the variation of baryon structure in matter also play important roles in supporting a massive neutron star.

X

In Kaluza-Klein electromagnetism it is natural to associate modified gravity with strong electromagnetic fields. Hence, in this paper we investigate the combined effects of a strong magnetic field and perturbative f(R) gravity on the structure of neutron stars. The effect of an interior strong magnetic field of about 1017?18 G on the equation of state is derived in the context of a quantum hadrodynamics (QHD) equation of state (EoS) including effects of the magnetic pressure and energy along with occupied Landau levels. Adopting a random orientation of interior field domains, we solve the modified spherically symmetric hydrostatic equilibrium equations derived for a gravity model with f(R) = R+?R2. Effects of both the finite magnetic field and the modified gravity are detailed for various values of the magnetic field and the perturbation parameter ? along with a discussion of their physical implications. We show that there exists a parameter space of the modified gravity and the magnetic field strength, in which even a soft equation of state can accommodate a large ( > 2 M?) maximum neutron star mass.