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| Kepler-10c was the first Kepler target to be observed using Spitzer with the hope of detecting a shallow transit dip in a light curve. At the time of Kepler-10c's discovery, Spitzer was the only facility capable of detecting shallow transits in the Kepler data to an extent at which the data could be meaningfully analyzed. The planet was also the third transiting planet that was validated through an analysis of statistical data (rather than actual observation), after the planets ] and ].<ref name=Fressin2011 /> In Kepler-10c's confirmation paper, the Kepler team discussed how a large fraction of planets in Kepler's field of view would be confirmed in this statistical manner.<ref name=Spitzy /> | Kepler-10c was the first Kepler target to be observed using Spitzer with the hope of detecting a shallow transit dip in a light curve. At the time of Kepler-10c's discovery, Spitzer was the only facility capable of detecting shallow transits in the Kepler data to an extent at which the data could be meaningfully analyzed. The planet was also the third transiting planet that was validated through an analysis of statistical data (rather than actual observation), after the planets ] and ].<ref name=Fressin2011 /> In Kepler-10c's confirmation paper, the Kepler team discussed how a large fraction of planets in Kepler's field of view would be confirmed in this statistical manner.<ref name=Spitzy /> | ||
| ==Host star== | |||
| {{main|Kepler-10}} | |||
| Kepler-10 is a ] star located 173 ]s (564 ]s) from Earth. The star is 0.895 ]es and 1.056 ], making the star slightly less massive than the Sun, but approximately the same size. With an ] of 5627 ], Kepler-10 is cooler than the Sun. The star is also metal-rich and far older: respectively, its ] is measured at = -0.16 (71% the amount of iron in the Sun), and its age at 11.9 billion years.<ref name=EPE /> | |||
| Kepler-10 has an ] of 10.96, which means that the planet is invisible to the ] from the perspective of an observer on Earth.<ref name=EPE /> | |||
| There are two planets known in the orbit of Kepler-10, the first being Kepler-10b. Kepler-10b is a rocky planet<ref name=Fressin2011 /> that orbits Kepler-10 every 0.8 days at a distance of 0.01684 ].<ref name=datatable /> | |||
| ==References== | ==References== | ||
Revision as of 17:25, 17 June 2011
Template:Planetbox begin Template:Planetbox star Template:Planetbox character Template:Planetbox orbit Template:Planetbox discovery Template:Planetbox end Kepler-10c is an exoplanet orbiting Kepler-10, located around 560 light-years away in Draco. Its discovery was announced by Kepler in May 2011; the team confirmed the observation using data from NASA's Spitzer Space Telescope.
Discovery and confirmation
sIn January 2011, some four months prior, the closely-orbiting planet Kepler-10b was confirmed in the orbit of the star Kepler-10 after measurements of its transiting behavior (where it crosses in front of Kepler-10, periodically dimming it) and a radial velocity effect detected in Kepler-10's spectrum provided the information needed to prove that it was indeed a planet. An additional, longer-period dimming was detected in Kepler-10's spectrum, suggesting that a second planet existed in the system; however, there remained the possibility that this signal could have been caused by some alternative reason, and that the transit event was a false positive. Attempts to measure the radial velocity effects of this object, now named KOI 072.02, were fruitless; therefore, to rule out false positive scenarios, the Kepler team used a technique called Blender.
The application of Blender was supplemented by use of the IRAC instrument on the Spitzer Space Telescope, which was used on August 30 and November 15 in 2010 to further define Kepler-10's light curve at the point where KOI 072.02 appeared to transit it. It was found that the transiting object did not produce a color, something characteristic of stars. This suggested even further that KOI 072.02 was a planet. In addition, the IRAC instrument found no difference in the transit signal when comparing the star's light curve in the infrared and in visible light; stars that are aligned with Kepler-10 might appear visibly similar, but would appear different in the infrared.
The WIYN Observatory's 3.5m telescope was used for speckle imaging on June 18, 2010; in addition, the PHARO camera on the Palomar Observatory's 5m telescope was used for its adaptive optics capabilities. These observations, combined with observations of Kepler-10's spectrum taken from the W.M. Keck Observatory, to rule out the possibility that a nearby star's light was corrupting the observed spectrum of Kepler-10 and creating the results that had led astronomers to believe that a second planet existed in Kepler-10's orbit. All of these possibilities, with the exception of if such a star existed exactly behind or in front of Kepler-10, were effectively ruled out; even with this, the Kepler team found that if a star was indeed aligned with Kepler-10 as seen from Earth, such a star would probably not be a giant star.
With a greater degree of certainty established, the Kepler team compared the models formed using Blender to the photometric observations collected by the Kepler satellite. The Blender technique allowed the Kepler team to rule out the majority alternatives including, notably, that of triple star systems. Blender then allowed the Kepler team to determine that although all models representing hierarchical triple stars (a binary system between a single star and a double star) can resemble the light curve of Kepler-10, the aforementioned follow-up observations would have detected them all. The only possible blends remaining after ruling out hierarchical triple stars was that of determining if the curve is caused by interference from a background star, or if it is indeed caused by the orbit of a transiting planet.
Comparisons of KOI 072.02 to the 1235 other Kepler Objects of Interest in Kepler's field of vision allowed astronomers to use models that led to the confirmation of KOI 072.02 as a planet with a high degree of certainty. KOI 072.02 was then renamed Kepler-10c. The planet's confirmation was announced at the Boston meeting of the American Astronomical Society on May 23, 2011.
Kepler-10c was the first Kepler target to be observed using Spitzer with the hope of detecting a shallow transit dip in a light curve. At the time of Kepler-10c's discovery, Spitzer was the only facility capable of detecting shallow transits in the Kepler data to an extent at which the data could be meaningfully analyzed. The planet was also the third transiting planet that was validated through an analysis of statistical data (rather than actual observation), after the planets Kepler-9d and Kepler-11g. In Kepler-10c's confirmation paper, the Kepler team discussed how a large fraction of planets in Kepler's field of view would be confirmed in this statistical manner.
Host star
Main article: Kepler-10Kepler-10 is a G-type star located 173 parsecs (564 light years) from Earth. The star is 0.895 solar masses and 1.056 solar radii, making the star slightly less massive than the Sun, but approximately the same size. With an effective temperature of 5627 K, Kepler-10 is cooler than the Sun. The star is also metal-rich and far older: respectively, its metallicity is measured at = -0.16 (71% the amount of iron in the Sun), and its age at 11.9 billion years.
Kepler-10 has an apparent magnitude of 10.96, which means that the planet is invisible to the naked eye from the perspective of an observer on Earth.
There are two planets known in the orbit of Kepler-10, the first being Kepler-10b. Kepler-10b is a rocky planet that orbits Kepler-10 every 0.8 days at a distance of 0.01684 AU.
References
- "Second rocky world makes Kepler-10 a multi-planet system", Leslie Mullen. Phys Org. May 26, 2011. Accessed June 10, 2011
- ^ "Kepler Discoveries". Ames Research Center. NASA. 2011. Retrieved 17 June 2011.
- ^ Jean Schneider (2011). "Notes for planet Kepler-10 c". Extrasolar Planets Encyclopaedia. Retrieved 17 June 2011.
- ^ "Kepler-10c and a New Method to Validate Planets". Ames Research Center. NASA. 2011. Retrieved 17 June 2011.
- ^ "Planet? Check". Jet Propulsion Laboratory. California Institute of Technology/NASA. 2011. Retrieved 17 June 2011.
- ^ Fressin, F.; Torres, G. (2011). "KEPLER-10C, A 2.2 EARTH RADIUS TRANSITING PLANET IN A MULTIPLE SYSTEM". Retrieved 17 June 2011.
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