Equation of state at high density and low temperature
High isospin asymmetric matter
High Energy Physics
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, 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
- Assistant Professor, Kent State University, Kent, Ohio, USA
- 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.