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

vdexheim {at}
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
  • Highly isospin asymmetric matter
  • Phase transitions
  • Neutron stars
  • Quark stars
  • Magnetars
  • General relativity
  • Supernova explosions
  • Compact Star Mergers
  • Hyperonic matter
  • Meson condensation
  • Color Superconductivity
  • Star Rotation and Cooling
High Energy Physics
  • QCD phase diagram
  • Chiral symmetry restoration
  • Deconfinement to quark matter

  • 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, Brazil ; Thesis topic: Nuclear Matter Compressibility in Neutron Stars
  • 2003 - BS Physics, Universidade Federal do Rio Grande do Sul, Porto Alegre, Brazil

Places I've worked
Associate Professor, Kent State University, Kent, Ohio, USA
Assistant Professor, Kent State University, Kent, Ohio, USA
Researcher, Universidade Federal de Santa Catarina, Florianopolis, Brazil
Visiting Assistant Professor, Gettysburg College, Gettysburg PA, USA
Adjunct Professor, Gettysburg College, Gettysburg PA, USA

Tabulated Equations of State
Information about CMF EoS
CompOSE EoS Instruction Manual
Tabulated CMF EoS (new column with leptonic chemical potential updated on Jul 20 2018, new tables with crust updated on Dec 10, 2018)
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 are hyperons, that contain non-zero strangeness and, if the density is high enough to deconfine them, quarks.

Below, astronomical objects containing extremely dense matter are shown in the QCD phase diagram (pink bubbles). On the vertical axis is the temperature and on the horizontal axis is the chemical potential (or density) of matter. The grey bubbles exemplify the early universe and different environments created in the lab.