Exoplanetology

Exoplanetology, or exoplanetary science, is an integrated field of astronomical science dedicated to the search and study of exoplanets (extrasolar planets). It employs an interdisciplinary approach which includes astrobiology, astrophysics, astronomy, astrochemistry, astrogeology, geochemistry, and planetary science.

Methodology

The first exoplanet was detected on 6 October 1995, and was named 51 Pegasi b. When extrasolar planets are observed to transit their parent stars, astronomers are able to assess some physical properties of the planets from an interstellar distance, including planetary masses and size, which in turn provide fundamental constraints on models of their physical structure. Furthermore, such events afford the opportunity to study the dynamics and chemistry of their atmospheres.

Statistical surveys and individual characterization are the keys to addressing the fundamental questions in exoplanetology. Varying techniques have been used to discover 2,002 planets outside the Solar System. Documenting the properties of a large sample exoplanets at various ages, orbiting their parent stars of various types, will contribute to increased understanding —or better models— of planetary formation (accretion), geological evolution, orbit migration, and their potential habitability. Characterizing the atmospheres of extrasolar planets is the new frontier in exoplanetary science.

Detection techniques

Main article: Methods of detecting extrasolar planets

About 97% of all the known exoplanets have been discovered by indirect techniques of detection, mainly by radial velocity measurements and transit monitoring techniques. The following methods have proved successful for discovering a new planet or confirming an already discovered planet:

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Habitability potential

See also: Astrobiology, Circumstellar habitable zone, and Planetary habitability

As more planets are discovered, the field of exoplanetology continues to grow into a deeper study of extrasolar worlds, and will ultimately tackle the prospect of life on planets beyond the Solar System. At cosmic distances, life can only be detected if it is developed at a planetary scale and strongly modified the planetary environment, in such a way that the modifications cannot be explained by classical physico-chemical processes (out of equilibrium processes). For example, molecular oxygen (O
₂) in the atmosphere of Earth is a result of photosynthesis by living plants and many kinds of microorganisms, so it can be used as an indication of life on exoplanets, although small amounts of oxygen could also be produced by non-biological means. Furthermore, a potentially habitable planet must orbit a stable star at a distance within which planetary-mass objects with sufficient atmospheric pressure can support liquid water at their surfaces.

See also

• Circumstellar habitable zone
• Lists of exoplanets
• List of exoplanet search projects
• Planetary science

External links

• Kepler public data archive by the Space Telescope Science Institute
• Strömgren Survey for Asteroseismology and Galactic Archaeology

Exoplanet catalogs and databases

• Extrasolar Planets Encyclopaedia by the Paris Observatory
• The Habitable Exoplanets Catalog by UPR Arecibo
• New Worlds Atlas by the NASA/JPL PlanetQuest