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| '''Kepler-91b''' is a planet orbiting ], star slightly more massive than the ]. Kepler-91 has left the main sequence and is now a ] star. | '''Kepler-91b''' is a planet orbiting ], star slightly more massive than the ]. Kepler-91 has left the main sequence and is now a ] star. | ||
| ==Discovery and further confirmation== | |||
| ==Claims for discovery== | |||
| Kepler-91b was detected by analyzing the data of ] where a transit-like signal was found. Initially thought to be a false positive due to light curve variations by a self-luminous object, it was later revealed that due low density of Kepler-91's shape is distorted to slightly ellipsoidal shape due to gravitational effects of the planet. Ellipsoidal light variations caused by Kepler-91b constitute more than the third of light variations compared to transit depth. Ellipsoidal light variations also allowed to determine the planet's mass. It was also found that Kepler-91b reflects some of the starlight from its star.<ref></ref> | Kepler-91b was detected by analyzing the data of ] where a transit-like signal was found. Initially thought to be a false positive due to light curve variations by a self-luminous object, it was later revealed that due low density of Kepler-91's shape is distorted to slightly ellipsoidal shape due to gravitational effects of the planet. Ellipsoidal light variations caused by Kepler-91b constitute more than the third of light variations compared to transit depth. Ellipsoidal light variations also allowed to determine the planet's mass. It was also found that Kepler-91b reflects some of the starlight from its star.<ref></ref> | ||
| Further analysis managed to question the planetary nature of the object. However, the planetary nature was eventually confirmed again. <ref name="arxiv">{{cite web|url=http://arxiv.org/abs/1401.1207|title=[1401.1207] A High False Positive Rate for Kepler Planetary Candidates of Giant Stars using Asterodensity Profiling|publisher=arxiv.org|accessdate=2014-01-20}}</ref> |
Further analysis managed to question the planetary nature of the object, suspecting that it is a self-luminous object. However, the planetary nature was eventually confirmed again. <ref name="arxiv">{{cite web|url=http://arxiv.org/abs/1401.1207|title=[1401.1207] A High False Positive Rate for Kepler Planetary Candidates of Giant Stars using Asterodensity Profiling|publisher=arxiv.org|accessdate=2014-01-20}}</ref> | ||
| ==Characteristics== | ==Characteristics== | ||
Revision as of 12:19, 10 July 2014
Template:Planetbox begin Template:Planetbox star Template:Planetbox character Template:Planetbox orbit Template:Planetbox discovery Template:Planetbox catalog Template:Planetbox end
Kepler-91b is a planet orbiting Kepler-91, star slightly more massive than the Sun. Kepler-91 has left the main sequence and is now a red giant branch star.
Discovery and further confirmation
Kepler-91b was detected by analyzing the data of Kepler spacecraft where a transit-like signal was found. Initially thought to be a false positive due to light curve variations by a self-luminous object, it was later revealed that due low density of Kepler-91's shape is distorted to slightly ellipsoidal shape due to gravitational effects of the planet. Ellipsoidal light variations caused by Kepler-91b constitute more than the third of light variations compared to transit depth. Ellipsoidal light variations also allowed to determine the planet's mass. It was also found that Kepler-91b reflects some of the starlight from its star.
Further analysis managed to question the planetary nature of the object, suspecting that it is a self-luminous object. However, the planetary nature was eventually confirmed again.
Characteristics
Kepler-91b is about 14% less massive than Jupiter while being more than 35% larger, making it less than half of the density of water. Kepler-91b orbits around the host star in about 6.25 days. Despite being one of the least edge-on orbits relative to Earth with inclination being about 68.5 degrees, transit was detected due to low semi-major axis to host star radius ratio.
Kepler-91b is expected to be engulfed by the parent star within about 55 million years.
References
- Kepler-91b: a planet at the end of its life. Planet and giant host star properties via light-curve variations
- "[1401.1207] A High False Positive Rate for Kepler Planetary Candidates of Giant Stars using Asterodensity Profiling". arxiv.org. Retrieved 2014-01-20.
- Kepler-91b: a planet at the end of its life. Planet and giant host star properties via light-curve variations J. Lillo-Box, D. Barrado, A. Moya, B. Montesinos, J. Montalbán, A. Bayo, M. Barbieri, C. Régulo, L. Mancini, H. Bouy, T. Henning: 14 Dec 2013
- http://arxiv.org/abs/1407.2245 Changing Phases of Alien Worlds: Probing Atmospheres of Kepler Planets with High-Precision Photometry] Lisa J. Esteves, Ernst J. W. De Mooij, Ray Jayawardhana: 10 Jul 2014
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