Equation of state at high density and low temperature
Highly isospin asymmetric matter
High Energy Physics
Compact Star Mergers
Star Rotation and Cooling
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
- 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
- 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 (more accurate results - updated on Dec 22, 2017)
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.