Revision as of 06:11, 4 April 2014 editHebrides (talk | contribs)Autopatrolled, Extended confirmed users, Pending changes reviewers105,192 edits →Claims for discovery: ref name using AWB← Previous edit | Revision as of 05:20, 10 July 2014 edit undoArtman40 (talk | contribs)2,039 edits Confirmed nowNext edit → | ||
Line 35: | Line 35: | ||
| discovery_method = ] (]) | | discovery_method = ] (]) | ||
| detection_methods = Ellipsoidal light variations <br> Reflection/emission modulations | | detection_methods = Ellipsoidal light variations <br> Reflection/emission modulations | ||
| discovery_status = |
| discovery_status = Confirmed}} | ||
}} | |||
{{Planetbox catalog | {{Planetbox catalog | ||
| names = KOI 2133.01 | | names = KOI 2133.01 | ||
Line 42: | Line 41: | ||
{{Planetbox end}} | {{Planetbox end}} | ||
'''Kepler-91b''' is |
'''Kepler-91b''' is a planet orbiting ], star slightly more massive than the ]. Kepler-91 has left the main sequence and is now a ] star. | ||
==Claims for discovery== | ==Claims for discovery== | ||
Line 48: | Line 47: | ||
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.<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. 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== | ||
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 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.<ref> 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</ref> | Kepler-91b is expected to be engulfed by the parent star within about 55 million years.<ref> 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</ref><ref>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</ref> | ||
==References== | ==References== |
Revision as of 05:20, 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.
Claims for discovery
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. 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
External links
2013 in space | ||||||
---|---|---|---|---|---|---|
Space probe launches |
| |||||
Impact events | ||||||
Selected NEOs | ||||||
Exoplanets |
| |||||
Discoveries |
| |||||
Novae | ||||||
Comets | ||||||
Space exploration |
| |||||
This extrasolar-planet-related article is a stub. You can help Misplaced Pages by expanding it. |