13 de Marzo de 2012
Serie de Clases Magistrales - DR. Joachim Puls 

Realizados por el Dr. Joachim Puls, proveniente de la U. de Munchen, Alemania, de visita en nuestro Centro de Astrofísica invitado por el Dr. Michel Curé. Los días 13, 15, 19 y 20 de Marzo, entre las 9.00 y 12.30 hrs.,  realizará cuatro Clases Magistrales tituladas "Radiation Driven Winds from Hot Massive Stars". El evetno esta dirigido a los Porfesores, Investigadores y alumnos de Postrado del Departamento de Física y Astronomía de la Facultad de Ciencias. Mas detalles sobre este evento

Director:
Radostin Kurtev

Investigadores:
Jura Borissova
Víctor Cárdenas
Michel Curé
Martin Gaskell
Ivan González
Verónica Motta
Matthias Schreiber
Claus Tappert
Nikolaus Vogt

Post-Docs:
James Clarke
Stuart Folkes
Alberto Rebassa
Gisela Romero
Samer Kanaan
Stuart Sale
Luis Vega
Mónica Zorotovic

No hay puestos vacantes
abiertos en este momento

Próximas charlas programadas:

Martes 03 de Abril de 2012, 14.00 hrs.

Auditorio de la Facultad de Ciencias
Dr. Nikolaus Vogt
Reunión del Grupo 07
Alumnos Carrera de Licenciatura en Fisica Mencion Astronomía

Pendiente
Auditorio de la Facultad de Ciencias.
Dr.  Samer Kanaan
Investigador Posdoctoral
PhD. Université de Nice Sophia-Antipolis, Francia.
"Stellar interferometry and its contribution to the study of Be and B[e] phenomena"
Be and B[e] stars exhibit infrared excess and emission lines in their spectra due to the presence of a circumstellar environment of gas and/or dust. Although they have common points their circumstellar environments are very different. In the case of Be stars the gaseous environment is often optically thin, whereas the dusty environment of B [e] stars is often optically thick. Many mechanisms to explain the ejection of matter from the photosphere were proposed such like the fast rotation, non-radial pulsations, radiative winds or binarity. This last one is the more likely scenario for B [e] stars, since they are not critical rotators as Be stars, and because it also allows the formation and the survival of their circumstellar environment on long term time scales. The lack of angular resolution in observations limited the study of these objects and  their modelling was based only on fitting the SED or line profiles. To discriminate between the various physical processes describing the mass loss and the distribution  of matter in the circumstellar medium, the geometry and the kinematics of these envelopes have to be fully constrained. This cannot be done by a single telescope and  ong-baseline interferometry is the only available technique to reach the spatial resolution necessary to resolve most of the envelopes. The VLTI instruments  AMBER (near IR 1-2.5 μm) and MIDI (mid IR 8-13 μm) are perfectly adapted to the study of these gaseous and dusty environments as their flux is generally dominated by  circumstellar emission beyond 1 μm

calendario de charlas futuras
y archivo de seminarios