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Silicon Photonics is the technological to face the future challenges in data communications and processing. This technology follows the same paradigm as the technological revolution of the integrated circuit industry, that is, the miniaturization and the standardization. One of the most important building blocks in Silicon Photonics is the microresonator, a circular optical cavity, which enables many different passive and active optical functions. Here, we will describe the new physics of the intermodal coupling, which occurs when multi radial mode resonators are coupled to waveguides, and of the optical chaos, which develops in coupled sequence of resonators. In addition, an application of resonators in the label-free biosensing will be discussed.
The CoRoT and Kepler space missions have opened a new era in eclipsing binary research. While specifically designed for exoplanet search, they offer as by-products the discovery and monitoring of variable stars, in great majority eclipsing binaries (EB). The missions are therefore providing thousands of EB light curves of unprecedented accuracy (typically a few hundred parts per million, ppm), with regular sampling (from 1s to 29m), extending over time spans of months, and with a very high duty cycle (>90%).
Thanks to this excellent photometry, research topics as asteroseismology of EB components are quickly developing, and physical phenomena such as doppler boosting, theoretically predicted but extremely difficult to observe from the ground, have been unambiguously detected. We present the main properties of the Corot and Kepler EB samples and briefly review the highlights of the missions in this field.
A large program of multi-fibre (FLAMES) spectroscopic observations of the stellar population in two CoRoT/Exoplanet field with the GIRAFFE/VLT, took place in spring 2008. It aims at characterizing the brightest dwarf population and providing the ground for statistical analysis of the planetary population found by CoRoT.
To perform such an ambitious analysis, we use an automated software based on the MATISSE algorithm, originally designed for the GAIA/RVS spectral analysis. This software derives the atmospheric stellar parameters: effective temperature, surface gravity and the overall metallicity.
Further improvements are foreseen in order to measure also individual abundances. By comparing the main physical and chemical properties of the host stars to those of the stellar population they belong to, this will bring new insights into the formation and evolution of exoplanetary systems and the star-planet connection.
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