Eventos

The direct detection of terrestrial extra-solar planned should be possible in the next 10 or 20 years. It is the main purpose of two space missions: Darwin (ESA) and TPF (NASA).

This talk deals with properties of very young (< 10-20 Myr) stellar clusters which are in the nebular phase and are embedded in photoionized regions (classical extragalactic HII regions (RHIIs) or starburst galaxies).

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In this seminar, an overview of the utility of studying non-radial non-adiabatic oscillations of stars such as $\delta$ Scuti, $\beta$ Cephei and Slowly Pulsating B stars will be given, with a particular attention on the problem of mode identification.

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The description and the first results of the new project will be presented. It is devoted to the search for the most metal-deficient blue compact galaxies.

LS-RCrA 1 es una estrella de tipo espectral muy tardío (M6.5-M7) cuyo espectro muestra líneas de emisión muy intensas, tanto prohibidas como permitidas.

According to the hierarchical scenario, galaxies form via merging and accretion of small objects. Within a series of high resolution simulations we have studied the formation and evolution of dark matter halos hosting galaxies. First halos have been formed at z > 10.

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We investigate effective 4-dimensional theories which were obtained under dimensional reduction of multidimensional cosmological models.

We have been observing a number of blazars with the Very Long Baseline Array in concert with monitoring at other wavebands, including X-rays and gamma-rays.

The comparative study of the planetary atmospheres is a young and interesting science, because of the diversity of the situations. As part of this programme, the exploration of Mars is very challenging.

El objetivo fundamental de esta charla es promover un acercamiento entre las comunidades observacional y teórica de este Instituto.

El principio de mínima interacción es revisado en un marco grupoteórico.

En esta charla se hará una revisión del concepto de corrugación como fenómeno universal que afecta a los discos de las galaxias espirales y se plantean diversas estrategias para dirimir su origen y estructura.

In (hopefully) 5 months ESA's polar platform ENVISAT will be launched. The Michelson Interferometer for Passive Atmospheric Sounding (MIPAS) is one of the core instruments and will continously record high resolution emission spectra of the Earth's atmosphere.

Because canonical neutron stars consist mainly of superfluid neutrons, superconducting protons and extremely relativistic electrons, all enclosed by a thin solid crust, the magnetic field structures of these stars vary in predictable ways during stellar spin-up and spin-down.

Los modelos dinámicos multifluido realizados hasta la fecha para el cálculo de la distribución de gas y polvo en las comas cometarias rodeando núcleos no esféricos no tienen en cuenta el efecto del "scattering" múltiple de la luz solar por las partículas que rodean al cometa.

There are two known reservoirs of water on Mars: the atmosphere, and the north polar cap. The latter contains possibly as much as 10 meters of water (global ocean equivalent). What happens to this water at high obliquity?

Seminario-coloquio

The debate about the possible smoothness of the Universe on large scales as opposed to an unbounded fractal hierarchy has been the subject of increasing interest in recent years. The controversy arises as a consequence of different statistical analyses performed on surveys of galaxy redshifts.

There exist isolated star complexes , located sometimes far away from the center of a galaxy or from the spiral arms. These complexes often have spheroidal or arc-like shapes. The best examples are in the LMC, NGC 6946 and NGC 5236.

We present old and new unpublished multiwavelength data for the most famous compact group of galaxies. Such groups are ideal laboratories for studying the effects of strong interactions.

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I present (WeCAPP) our long time project searching for microlensing events in M31. Since 1997 the bulge of M31 was monitored in two different wavebands with the Wendelstein 0.8 m telescope. In 1999 we extended our observations to the Calar Alto 1.23m telescope.

En esta charla trataré de repasar y resumir nuestros conocimientos más actuales acerca del campo magnético de las manchas, de su estructura tridimensional, del transporte energético a través de su atmósfera, así como de las relaciones del campo magnético con los fenómenos dinámicos más importante