Detection and characterization of Earth-like planets

Details Detection and characterization of Earth-like planets Detection and characterization of Earth-like planets

Jan 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997abos.conf..299m&link_type=abstract

Conference Paper, Astronomical and Biochemical Origins and the Search for Life in the Universe, IAU Colloquium 161, Publisher: B

Astronomy and Astrophysics

Astronomy

1

Extrasolar Planets, Earth (Planet), Radial Velocity, Astrometry, Infrared Spectra, Planetary Atmospheres, Planetology, Occultation, Infrared Interferometers, Coronagraphs, Extraterrestrial Life

Scientific paper

Indirect methods of detection of exoplanets (by radial velocity, astrometry, occultations, etc.) have recently revealed the first cases of exoplanets, and will in the near future expand our knowledge of these systems. They will provide statistical information on such dynamical parameters as semimajor axis, eccentricities, and inclinations. To characterize Earth-like exoplanets in greater detail, direct detection (i.e., direct observation of photons from the planet) is required. The exoplanets are extremely faint with respect to their star: the contrast ratio is about 10 exp -10 at visible wavelengths. Also, the angular size of the apparent orbit Js small, typically 0.1 arcsec. While the first point calls for observations in the IR (where the contrast goes up to 10 exp -7) and with a coronograph, the latter implies using an interferometer. Several space projects combining these techniques have recently been proposed. They aim at surveying several hundred nearby single solarlike stars in search of Earth-like planets, and at performing a low-resolution spectroscopic analysis of their IR emission in order to reveal the presence of CO, H2O, and O3 in the atmosphere of the planet.

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