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.
The first exoplanet was detected in 6 October 1995, and was named 51 Pegasi b. When extrasolar planets are observed to transit their parent stars, astronomers are granted unprecedented access to their physical properties, such as planetary masses and size, which in turn provide fundamental constraints on models of their physical structure. Furthermore, such planets 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. Through May 2015, varying techniques have been used to discover 1,924 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.
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: 
- Radial velocity
- Gravitational microlensing
- Direct imaging
- Reflection/emission modulations
- Light variations due to relativistic beaming
- Light variations due to ellipsoidal variations
- Pulsar timing
- variable star timing
- Transit timing variation method
- Transit duration variation method
- Eclipsing binary minima timing
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 indication of life on exoplanets, although 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.
- Exoplanet Anniversary: From Zero to Thousands in 20 Years. NASA News, 6 October 2015.
- "The Era of Comparative Exoplanetology." American Astronomical Society. Charbonneau, David. AAS Meeting #212, #54.01; Bulletin of the American Astronomical Society, May 2008, Vol. 40, p.250
- Interactive Extra-solar Planets Catalog, The Extrasolar Planets Encyclopaedia. Updated Sept 30, 2010. Accessed October 2, 2010.
- Ollivier M., Encrenaz T., Roques F., Selsis F., Casoli F., Planetary Systems - Detection, Formation and Habitability of Extrasolar Planets, Springer, Berlin (2008)
- public data archiveKepler 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