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| {{Planetbox begin | {{Planetbox begin | ||
| | name=Kepler-91b | | name = Kepler-91b | ||
| }} | }} | ||
| {{Planetbox star | {{Planetbox star | ||
| | star = ] | | star = ] | ||
| | constell = ] | | constell = ]<ref name="Roman1987"/> | ||
| | RA = {{RA|19|02|41.0}} | | RA = {{RA|19|02|41.0}} | ||
| | DEC = {{DEC|+44|07|00}} | | DEC = {{DEC|+44|07|00}} | ||
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| ==Discovery and further confirmation== | ==Discovery and further confirmation== | ||
| 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 name="Lillo-Box">{{Cite journal|arxiv=1312.3943|last1= Lillo-Box|first1= J.|title= Kepler-91b: A planet at the end of its life. Planet and giant host star properties via light-curve variations|journal= Astronomy & Astrophysics|volume= 562|pages= A109|last2= Barrado|first2= D.|last3= Moya|first3= A.|last4= Montesinos|first4= B.|last5= Montalbán|first5= J.|last6= Bayo|first6= A.|last7= Barbieri|first7= M.|last8= Régulo|first8= C.|last9= Mancini|first9= L.|last10= Bouy|first10= H.|last11= Henning|first11= T.|year= 2013|doi= 10.1051/0004-6361/201322001|bibcode= 2014A&A...562A.109L}}</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 name="Lillo-Box">{{Cite journal|arxiv=1312.3943|last1= Lillo-Box|first1= J.|title= Kepler-91b: A planet at the end of its life. Planet and giant host star properties via light-curve variations|journal= Astronomy & Astrophysics|volume= 562|pages= A109|last2= Barrado|first2= D.|last3= Moya|first3= A.|last4= Montesinos|first4= B.|last5= Montalbán|first5= J.|last6= Bayo|first6= A.|last7= Barbieri|first7= M.|last8= Régulo|first8= C.|last9= Mancini|first9= L.|last10= Bouy|first10= H.|last11= Henning|first11= T.|year= 2013|doi= 10.1051/0004-6361/201322001|bibcode= 2014A&A...562A.109L}}</ref> | ||
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| ==References== | ==References== | ||
| {{reflist|refs= | |||
| <ref name="Roman1987">{{cite journal | title=Identification of a Constellation From a Position | url=http://articles.adsabs.harvard.edu/full/1987PASP...99..695R | last1=Roman | first1=Nancy G. | journal=Publications of the Astronomical Society of the Pacific | volume=99 | issue=617 | pages=695–699 | date=1987 | bibcode=1987PASP...99..695R | doi=10.1086/132034 }} </ref> | |||
| }} | |||
| ==External links== | ==External links== | ||
Revision as of 00:09, 11 December 2017
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
- ^ Lillo-Box, J.; Barrado, D.; Moya, A.; Montesinos, B.; Montalbán, J.; Bayo, A.; Barbieri, M.; Régulo, C.; Mancini, L.; Bouy, H.; Henning, T. (2013). "Kepler-91b: A planet at the end of its life. Planet and giant host star properties via light-curve variations". Astronomy & Astrophysics. 562: A109. arXiv:1312.3943. Bibcode:2014A&A...562A.109L. doi:10.1051/0004-6361/201322001.
- Sliski, David H.; Kipping, David M. (2014). "A High False Positive Rate for Kepler Planetary Candidates of Giant Stars using Asterodensity Profiling". The Astrophysical Journal. 788 (2): 148. arXiv:1401.1207. Bibcode:2014ApJ...788..148S. doi:10.1088/0004-637X/788/2/148.
- Cite error: The named reference
Esteveswas invoked but never defined (see the help page). - Placek, Ben; Knuth, Kevin H.; Angerhausen, Daniel; Jenkins, Jon M. (2015). "Characterization of Kepler-91b and the Investigation of a Potential Trojan Companion Using EXONEST". The Astrophysical Journal. 814 (2): 147. arXiv:1511.01068. Bibcode:2015ApJ...814..147P. doi:10.1088/0004-637X/814/2/147.
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