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| | stellar_flux = | | stellar_flux = | ||
| | density_cgs = 0.44 | | density_cgs = 0.44 | ||
| | geometric_albedo = 0.39 <ref>{{ |
| geometric_albedo = 0.39 <ref>{{Cite journal|arxiv=1407.2245|last1= Esteves|first1= Lisa J.|title= Changing Phases of Alien Worlds: Probing Atmospheres of Kepler Planets | ||
| with High-Precision Photometry|journal= The Astrophysical Journal|volume= 804|issue= 2|pages= 150|last2= De Mooij|first2= Ernst J. W.|last3= Jayawardhana|first3= Ray|year= 2014|doi= 10.1088/0004-637X/804/2/150}}</ref> | |||
| | temperature = {{val|2132|u=K}} | | temperature = {{val|2132|u=K}} | ||
| }} | }} | ||
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| 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 to 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 to 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, suspecting that it is a self-luminous object. However, the planetary nature was eventually confirmed again.<ref name="arxiv">{{ |
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 journal|arxiv=1401.1207|title=[1401.1207] A High False Positive Rate for Kepler Planetary Candidates of Giant Stars using Asterodensity Profiling|journal=The Astrophysical Journal|volume=788|issue=2|pages=148|last1= Sliski|first1=David H.|last2= Kipping|first2=David M.|year=2014|doi=10.1088/0004-637X/788/2/148}}</ref> | ||
| ==Characteristics== | ==Characteristics== | ||
Revision as of 02:17, 12 July 2016
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, a 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 to 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.
Possible trojan companion
The possibility of a trojan planet to Kepler-91b was studied but the conclusion was that the transit-signal was a false-positive.
References
- Kepler-91b: a planet at the end of its life. Planet and giant host star properties via light-curve variations
- Sliski, David H.; Kipping, David M. (2014). "[1401.1207] A High False Positive Rate for Kepler Planetary Candidates of Giant Stars using Asterodensity Profiling". The Astrophysical Journal. 788 (2): 148. arXiv:1401.1207. doi:10.1088/0004-637X/788/2/148.
- 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
- 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
- Characterization of Kepler-91b and the Investigation of a Potential Trojan Companion Using EXONEST, Ben Placek, Kevin H. Knuth, Daniel Angerhausen, Jon M. Jenkins, (Submitted on 3 Nov 2015)
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