Instituto de Física y Astronomía

Cataclysmic variables (CVs) are binary stars where the less massive component,  a late-type (K-M) main-sequence star, transfers matter to the more massive component, a white dwarf. As such they represent a subclass of compact binaries. These objects show a large variety of phenomena, and their study bears relevance for several other areas of research, such as binary formation and evolution, accretion discs, or supernova progenitors.

Classical novae represent a subclass of CVs. The accumulation of a certain
critical amount of material on the white dwarf causes a thermonuclear explosion on its surface. In its course, material is expelled from the white dwarf into  the interstellar medium as a shell. This phenomenon is known as a 'nova  eruption'. Since the explosion does not destroy the binary system, the  accretion process recommences within one or two years. Thus, it is reasonable  to assume that the nova eruption represents a recurrent phenomenon and that it  forms part of the evolution of most, if not all, CVs.

At the IFA we currently study the following aspects of the physics of CVs: - the connection between the group of classical novae and other subtypes of CVs. We have initiated a search to recover former novae in order to  significantly enlarge the sample of such objects. This will allow for a statistically significant comparison of the properties of the 'post-novae' with those of 'other' CVs, and ultimately reveal both the importance of certain physical parameters on the nova eruption and the effect of the latter on them.      
- the long-term photometric behaviour of specific objects with the goal to gain information from their variability on the processes in their accretion
discs.

Investigators:

Professors: Claus Tappert - Dr. Nikolaus Vogt - Dr. Matthias Schreiber

La investigación del Centro de Astrofísica, en Planetas y Formación Estelar cubre las siguientes áreas:

Discos Protoplanetarios

Investigadores:

Docentes: Matthias Schreiber - Jura Borissova - Radostin Kurtev - Nikolaus Vogt - Amelia Bayo

Our team studies massive stars in general and Be, B[e] and SG in particular. Our approach is both theoretical and observational.

M. Curé is responsible for the theoretical part where he studies and develops different hydrodynamical methods to study winds and mass loss. Our team is expert in developing codes such as HydWind as well as using and ameliorating different state of the art codes such as SIMECA, MC3D, FastWind, CMFGEN and HDUST.

Responsible in the applications part is S. Kanaan where different observations programs are active in order to understand the mass loss of massive stars in general and Be and B[e] stars disk formation in particular.
In the observational part we are conducting a spectroscopic survey on Be stars as well as interferometric (VLTI) observations in order to constrain the disk geometry and its Kinematics.

Our group is working with different collaborators from around the globe combining theory and observations which will allow us to better understand these fascinating objects that play an important role in the enrichment of our Universe by heavy elements as well as the understanding of star evolution

Investigators:

Professors:  Jura Borissova - Matthias Schreiber - Samer Kanaan - Michel Curé