Colloquia and Seminars

Dr. Farrukh Fattoyev obtained his B.Sc in Physics from the Samarkand State University (Uzbekistan) in 2002 and his M.Sc. degree in Theoretical Physics from the National University of Uzbekistan in 2004. For his masters dissertation he studied the effect of spacetime curvature on some select electromagnetic processes. He then spent a year in the Institute of Nuclear Physics, Tashkent, Uzbekistan as a research assistant before continuing his education at an advanced masters program of Laurea Magistralis in the International Centre for Theoretical Physics (ICTP) and the University of Trieste. His masters dissertation at ICTP was on Theoretical Cosmology, for which he studied a generalized version of the slow-roll approach in cosmic inflation. Dr. Fattoyev went on to Florida State University to pursue a PhD in Theoretical Nuclear Physics under the supervision of Professor Jorge Piekarewicz on the sensitivity of the properties of neutron stars to the nuclear equations of state. After receiving his PhD in 2011 he joined the Department of Physics and Astronomy at Texas A&M University-Commerce in January, 2012 as a postdoc and is currently working with Prof. Bao-An Li and Prof. William Newton. His research interests are in theoretical nuclear physics and nuclear astrophysics that includes developing nuclear energy density functionals in the context of the relativistic mean-field (RMF) approach, the equation of state of nuclear matter at high densities and with large isospin asymmetries, density dependence of the nuclear symmetry energy, structure and composition of neutron stars, and testing sensitivity of various neutron star properties (mass versus radius relation, cooling processes, moments of inertia, tidal polarizability, gravitational waves, etc.) to the underlying equation of state. Dr. Fattoyev can be reached by email at farrooh.fattoyev@tamuc.edu and his publications can be found at http://scholar.google.com/citations?user=me4MZvUAAAAJ&hl=en

Abstract:

Neutron stars are fascinating stellar compact objects that are produced at the endpoint of stellar evolution. They provide natural laboratories to explore diverse physical phenomena in astrophysics, general relativity, atomic and nuclear physics. The structure, dynamics, and composition of neutron stars are very sensitive to the equation of state (EOS) of neutron-rich matter. A particular feature of the EOS is the nuclear symmetry energy, a quantity that encodes the energy cost of converting protons to neutrons as one departs from the symmetric limit of equal number of neutrons and protons. To date it is one of the most uncertain properties of dense, neutron-rich nucleonic matter, while has important consequences for many interesting questions in both nuclear physics and astrophysics. In this colloquium I will give a brief overview of historical introduction to neutron stars and discuss the role that the nuclear symmetry energy plays in understanding the structure and composition of neutron stars. In particular, I will focus on the impact of the nuclear symmetry energy to the various properties of neutron stars such as moments of inertia, crust-core transition properties, cooling processes, and gravitational wave signals. 

Colloquia will now be announced internally, only.