The Astrophysics group of IFIR ( Physics Institute of Rosario) is interested in the astrophysics study of the collapsed bodies such as neutron stars, strange matter stars, X and Gamma rays binaries, also in the dynamics of the stellar systems.

Group Members

• Dr. Roberto Aquilano
  Director del Grupo Investigador Independiente CONICET, Profesor Adjunto (ded. Semiexclusiva), Investigador Categoría I (Programa Incentivos)
• Dra. Miriam Scancich
  Jefe de Trabajos Prácticos (ded. Exclusiva), Investigador Categoría IV (Programa de Incentivos)
• Dr. Luis Pedro Neira
  Personal Municipal, Investigador Adscripto
• Dra. Edith Losada
  Becaria Posdoctoral de CONICET
• Lic. Alejandra Zorzi
  Becaria de CONICET
• Lic. Gabriel Perren
  Becario de CONICET
• Lic. Anabela Turlione
  Becaria de CONICET
• Lic. Martín Mestre
  Becario de CONICET
• Lic.. Diego Sevilla
  Becario de CONICET
• Srta. Silvia Morales
  Tesista
• Prof. Sergio Acero
  Personal de Apoyo Municipal
• Dr. Daniel Davoli
  Personal de Apoyo Municipal
• Téc. Hugo Missio
  Personal de Apoyo Municipal
• Téc. Juan Olivero
  Personal de Apoyo Municipal

Financial Center:

Project 1:

The description of hydrodynamics process, using General Relativity, specially in the gravitational collapse, is conditioned by two hypothesis: the state equation and the methods to solve Einstein´s equation. Because of that, it´s quite complex to obtain the evolution of a system for the relativistic state equation without considering spherical symmetry. So, we use methods to obtain models to describe radianting spheres but non static.
These methods are applied to astronomical objects such as X and Gamma Ray bursters, recurrent novaes, star binary systems, neutron stars, strange matter stars and supernovaes. Besides, the study takes into account new physical factors, like thermal conductivity of fluid, viscous fluids, anisotropic state equations, hydrodynamics phase transitions, surface phenomenon, etc.

PROJECT 2

Although, the construction of selfgraviting spheric stellar model system or disck form in an stable equilibrium is very simple, the triaxial systems, which are good enough to describe elliptic galaxies, are very much more complicated. We use classical methods to construct triaxial models and others methods of N-bodies codes, that make use of distributions which are not equilibrated, to follow the evolution to obtain systems which are in stable equilibrium.
Considering the positions and speeds (velocities) of N-bodies, it can be obtained their orbits and, for example, their Lyapunov exponents to predict chaos.