Difference between revisions of "Extrasolar planets"
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| − | '''Extrasolar planets''' or '''exoplanets''' are planets that orbit stars other than the sun. | + | [[File:G1758.jpg|thumb|250px||right|The first photo taken of an exoplanet, by the Japanese "Subaru" telescope, August, 2009. Point "B", numbered GJ758 B, has a mass of 10 to 40 times Jupiter, and orbits a star 50 light years from Earth. Point "C" (GJ758 C) is undetermined.<ref>http://www.space.com/7629-photo-object-sun-star-scientists.html</ref>]] |
| + | '''Extrasolar planets''', or '''exoplanets''', are planets that orbit stars other than the sun. The search for them is one of the most exciting phases of astronomy today. | ||
| − | Planets have no light source of their own, and most extrasolar planets are too far away to be seen by the light they reflect from their own suns | + | Planets have no light source of their own, and most extrasolar planets are too far away to be seen by the light they reflect from their own suns; however, over 400 have been detected with indirect methods, such as Doppler spectroscopy (determining the "wobble" of the parent star due to the orbiting planet's gravitational tug) or transit photometry (measuring the ever-so-slight dimming of the parent star when the planet passes through the line of sight, obscuring part of the star). Actually photographing the planet's faint speck of light against the host star's overwhelming glare is much more challenging, yet ultimately more rewarding because it provides critical information about the planet's orbit and the temperature and composition of its atmosphere. |
== Methods of detection == | == Methods of detection == | ||
=== Astrometry === | === Astrometry === | ||
| − | A star and planet orbit about a spot that is the center of gravity of the system known as the [[barycenter]]. For the Sun and Jupiter, the barycenter is 1.068 solar radii. With larger planets orbiting closer to the star, it is possible to detect the movement of the star against the distant background. This method was used to detect a planet orbiting Gliese 876. | + | A star and planet orbit about a spot that is the center of gravity of the system known as the [[orbit|barycenter]]. For the Sun and Jupiter, the barycenter is 1.068 solar radii. With larger planets orbiting closer to the star, it is possible to detect the movement of the star against the distant background. This method was used to detect a planet orbiting Gliese 876. |
=== Radial velocity === | === Radial velocity === | ||
| − | Instead of mapping the position of the star against the background, it is also possible to detect the minute [[Doppler shift]] in the star's spectrum as it is tugged by the planet. This method is responsible for the majority of extrasolar planet detection. | + | Instead of mapping the position of the star against the background, it is also possible to detect the minute [[Doppler effect|Doppler shift]] in the star's spectrum as it is tugged by the planet. This method is responsible for the majority of extrasolar planet detection. |
=== Transit method === | === Transit method === | ||
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=== Direct imaging === | === Direct imaging === | ||
In the situation where a star is not extremely bright, it is possible to detect a planet orbiting it. Such was the case with the brown dwarf 2M1207 which had a detectable companion that was named 2M1207b. | In the situation where a star is not extremely bright, it is possible to detect a planet orbiting it. Such was the case with the brown dwarf 2M1207 which had a detectable companion that was named 2M1207b. | ||
| + | |||
| + | On November 13, 2008 a planet orbiting the star [[Fomalhaut b|Fomalhaut]] at a distance of approximately 115 AU became the first exoplanet observed directly in visible light. The planet, whose existence was theoretically predicted, was photographed by the Hubble Space Telescope. It is believed to be a few times the mass of Jupiter and to posess an extrensive ring system. | ||
== Current count == | == Current count == | ||
| − | As of | + | As of February 2014, the number of extrasolar planets detected stands at about 1,700, with NASA announcing (February 26) that the Kepler Telescope had discovered 715 during the previous year.<ref>https://www.foxnews.com/science/2014/02/27/nasa-announces-mother-lode-new-planets-715/</ref><ref>http://www.space.com/24824-alien-planets-population-doubles-nasa-kepler.html</ref> Since the detection methods devised to date favor large, gaseous planets, most of the detected planets are quite dissimilar to Earth, and they are not thought to be good candidates for finding life. However, the planet [[Gliese 581c]] orbiting the red dwarf star Gliese 581 (approximately 20 light-years from earth) appears to be a terrestrial, i.e. rocky, planet that orbits in the "[[habitable zone]]" of space surrounding its star. |
| + | |||
| + | ==See also== | ||
| + | *[[Extraterrestrial life]] | ||
| + | *[[Essay: Extraterrestrial Life and the Bible]] | ||
| + | *[[Exotheology]] | ||
| + | ==Further reading== | ||
| + | * Thalmann, Christian, et al. "Discovery of the Coldest Imaged Companion of a Sun-Like Star," [https://arxiv.org/abs/0911.1127 submitted for publication, Nov. 2009], on the Subaru discovery | ||
| + | |||
| + | ==References== | ||
| + | {{Reflist}} | ||
| + | |||
| + | ==Links== | ||
| + | *[http://planetquest.jpl.nasa.gov/ NASA's PlanetQuest] | ||
| + | *[http://exoplanet.eu/ Extrasolar Planets Encyclopaedia] | ||
| + | *[http://exoplanets.org/ ExoPlanets] | ||
| + | *[http://www.subarutelescope.org/Pressrelease/2009/12/03/index.html"Discovery of an Exoplanet Candidate Orbiting a Sun-Like Star: Inaugural Observations with Subaru's New Instrument HiCIAO" Dec. 3, 2009] Subaru Press release | ||
| + | *[https://www.relativitycalculator.com/radial_velocity_equation.shtml The Radial Velocity Equation in the Search for Exoplanets ( The Doppler Spectroscopy or Wobble Method )] | ||
| + | |||
| + | |||
| + | {{Exo-Planets}} | ||
| − | [[ | + | [[Category:Astronomy]] |
Latest revision as of 12:01, April 9, 2019
Extrasolar planets, or exoplanets, are planets that orbit stars other than the sun. The search for them is one of the most exciting phases of astronomy today.
Planets have no light source of their own, and most extrasolar planets are too far away to be seen by the light they reflect from their own suns; however, over 400 have been detected with indirect methods, such as Doppler spectroscopy (determining the "wobble" of the parent star due to the orbiting planet's gravitational tug) or transit photometry (measuring the ever-so-slight dimming of the parent star when the planet passes through the line of sight, obscuring part of the star). Actually photographing the planet's faint speck of light against the host star's overwhelming glare is much more challenging, yet ultimately more rewarding because it provides critical information about the planet's orbit and the temperature and composition of its atmosphere.
Contents
Methods of detection
Astrometry
A star and planet orbit about a spot that is the center of gravity of the system known as the barycenter. For the Sun and Jupiter, the barycenter is 1.068 solar radii. With larger planets orbiting closer to the star, it is possible to detect the movement of the star against the distant background. This method was used to detect a planet orbiting Gliese 876.
Radial velocity
Instead of mapping the position of the star against the background, it is also possible to detect the minute Doppler shift in the star's spectrum as it is tugged by the planet. This method is responsible for the majority of extrasolar planet detection.
Transit method
When a planet passes in front of its star, it blocks some of the light of the star. By measuring this periodic momentary dimming of the light, it is possible to identify a planet that is properly aligned. This method does not work if the planet itself does not eclipse the star from our perspective.
Direct imaging
In the situation where a star is not extremely bright, it is possible to detect a planet orbiting it. Such was the case with the brown dwarf 2M1207 which had a detectable companion that was named 2M1207b.
On November 13, 2008 a planet orbiting the star Fomalhaut at a distance of approximately 115 AU became the first exoplanet observed directly in visible light. The planet, whose existence was theoretically predicted, was photographed by the Hubble Space Telescope. It is believed to be a few times the mass of Jupiter and to posess an extrensive ring system.
Current count
As of February 2014, the number of extrasolar planets detected stands at about 1,700, with NASA announcing (February 26) that the Kepler Telescope had discovered 715 during the previous year.[2][3] Since the detection methods devised to date favor large, gaseous planets, most of the detected planets are quite dissimilar to Earth, and they are not thought to be good candidates for finding life. However, the planet Gliese 581c orbiting the red dwarf star Gliese 581 (approximately 20 light-years from earth) appears to be a terrestrial, i.e. rocky, planet that orbits in the "habitable zone" of space surrounding its star.
See also
Further reading
- Thalmann, Christian, et al. "Discovery of the Coldest Imaged Companion of a Sun-Like Star," submitted for publication, Nov. 2009, on the Subaru discovery
References
Links
- NASA's PlanetQuest
- Extrasolar Planets Encyclopaedia
- ExoPlanets
- "Discovery of an Exoplanet Candidate Orbiting a Sun-Like Star: Inaugural Observations with Subaru's New Instrument HiCIAO" Dec. 3, 2009 Subaru Press release
- The Radial Velocity Equation in the Search for Exoplanets ( The Doppler Spectroscopy or Wobble Method )
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