Veronica Dexheimer
Veronica Dexheimer
Assistant Professor
Department of Physics
Kent State University
Kent, OH 44242 USA

vdexheim {at} kent.edu
Office: 209 Smith Hall
Phone: +1.330.672.2596
Fax: +1.330.672.2959
My Publications

Curriculum Vitae

Research Interests

Nuclear Physics
  • Equation of state at high density and low temperature
  • High isospin asymmetric matter
  • Phase transitions
Astrophysics
  • Neutron stars
  • Quark stars
  • Magnetars
  • General relativity
  • Supernova explosions
  • Hyperonic matter
  • Meson condensation
  • Star Rotation and Cooling
High Energy Physics
  • QCD phase diagram
  • Chiral symmetry restoration
  • Deconfinement to quark matter

Education
  • 2009 - PhD Physics, Frankfurt Institute for Advanced Studies, Johann Wolfgang Goethe University - Frankfurt an Main, Germany ; Dissertation topic Chiral Symmetry Restoration and Deconfinement in Neutron Stars
  • 2006 - MS Physics, Universidade Federal do Rio Grande do Sul, Porto Alegre, RS, Brasil ; Thesis topic: Nuclear Matter Compressibility in Neutron Stars
  • 2003 - BS Physics, Universidade Federal do Rio Grande do Sul, Porto Alegre, RS, Brasil

Places I've worked
2013-Present
Assistant Professor, Kent State University, Kent, Ohio, USA
2008-2012
Visiting Assistant Professor, Gettysburg College, Gettysburg, Pennsylvania, USA
Jan 2012-Aug 2012
Postdoctoral Researcher, Universidade Federal de Santa Catarina, Florianopolis, SC, Brasil
 
Matter at Extreme Densities

Neutron stars are very dense objects. One teaspoon of their material would have a mass of five billion tons. Their gravitational force is so strong that if an object were to fall from just one meter high it would hit the surface of the respective neutron star at 2 thousand kilometers per second. In such dense bodies, different particles from the ones present in atomic nuclei, the nucleons, can exist. These particles can be hyperons, that contain non-zero strangeness, or broader resonances. There can also be different states of matter inside neutron star, such as meson condensates and if the density is high enough to deconfine the nucleons, quark matter. As new degrees of freedom appear in the system, different aspects of matter have to be taken into account.

In the picture above I show a hypothetical cross section of the composition of a neutron star.

In the picture above I show the phase diagram for matter. On the vertical axis is the temperature and on the horizontal axis is the density of the matter.