Titlebook: Infrared Space Interferometry: Astrophysics & the Study of Earth-Like Planets; Proceedings of a Wor C. Eiroa,A. Alberdi,C. J. Schalinski Co

專(zhuān)橫

High Resolution Spectroscopy of Vega-Like Starsvidence either of high-velocity outflowing gas, variability in the circumstellar lines observed or evidence of circumstellar gas in excited lines of Fe II. No previous identification of circumstellar material has been made for two of the stars in question.

勛章

lethal

Infrared Observations of Planetary Atmospheresces of noise (apart from the detector noise) can be completely removed, the required integration time for detecting an Earth-like planet at 5 parsec (assuming the performances of the ISO detectors) is about two weeks for a 5-m telescope (R=100, S/N=5). Improving the sensitivity of the detectors would reduce these integration times accordingly.

narcissism

Detection of Planetary Spectral Features through Circumstellar Dust — A Monte Carlo Simulationing a central star of solar luminosity and temperature. The disk structure and the grain model resemble real properties in protoplanetary disks. The model was calculated for a set of different optical depths at various positions of the observer with respect to the configuration, the detectability of the embedded planetary sources is discussed.

Condescending

Planets in CM Draconis: A Multi-Site Photometric Search-band filters (V and R) and maintaining always common reference stars between all the observatories. So far, we have obtained about 500 hours of effective integration time on CM Dra, distributed in ～ 16000 CCD frames. We have analysed about 40% of the 94–95 database, and have found encouraging, albeit inconclusive, results.

微粒

dainty

0067-0057 lar system. Only a half-year before our meeting in Toledo, Spain, the first unambiguous detection of planet-sized masses orbiting main sequence stars were reported. Since that time, evidence for a new exo- planet has been reported almost at the rate of about once per month. Some of these objects are

majestic

動(dòng)脈

Array Configurations to Detect and Characterize Extrasolar Planets with a Space Infrared Interferomet many distinctive frequencies. A simple cross correlation method recovers a single image of a solar systemtwin at 10 pc distance, in about 30h. The spectroscopy of the planets can then be undertaken with the same baseline and would reveal absorption features of water, ozone and carbon dioxide of an

headway

Ground-Based Optical/IR Long Baseline Interferometryrby stars down to ～ 10 Earth masses and the use of the large telescopes planned for the end of the century should even permit direct detection of massive or young planets and brown dwarfs identified by radial velocity techniques. Thus, ground-based interferometers will represent powerful and versati