Planet KELT-15 b
| Name | KELT-15 b | ||
| Planet Status | Confirmed | ||
| Discovered in | 2015 | ||
| Mass | 0.92 ( -0.23 +0.23 ) MJ | ||
| Mass*sin(i) | 0.91 ( -0.22 +0.22 ) MJ |  |
|
| Semi-Major Axis | 0.04613 (± 0.00065) AU | |
|
| Orbital Period | 3.329441 (± 1.6e-05) day | |
|
| Eccentricity | — | ||
| ω | — | ||
| Tperi | — | ||
| Radius | 1.443 ( -0.057 +0.11 ) RJ | |
|
| Inclination | 79.67 (± 0.8) deg | |
|
| Update | 2018-12-17 | ||
| Detection Method | Primary Transit | ||
| Mass Detection Method | Radial Velocity | ||
| Radius Detection Method | Primary Transit | ||
| Primary transit | 2457091.02863 (± 0.00047) JD | |
|
| Secondary transit | 2457027.5016 ( -0.0073 +0.0078 ) JD | |
|
| λ | — | ||
| Impact Parameter b | 0.2 ( -0.14 +0.18 ) | ||
| Time Vr=0 | — | ||
| Velocity Semiamplitude K | 110.0 (± 26.0) m/s | ||
| Calculated temperature | — | ||
| Measured temperature | — | ||
| Hottest point longitude | — | ||
| Geometric albedo | — | ||
| Surface gravity log(g/gH) | — | ||
| Alternate Names | — |
Star
KELT-15| Name | KELT-15 | ||
| Distance | 201.0 (± 19.0) pc | |
|
| Spectral type | |||
| Apparent magnitude V | 11.44 | ||
| Mass | 1.181 (± 0.05) MSun | |
|
| Age | — | ||
| Effective temperature | 6003.0 (± 50.0) K | |
|
| Radius | 1.481 ( -0.041 +0.091 ) RSun | |
|
| Metallicity [Fe/H] | 0.047 (± 0.032) | |
|
| Detected Disc | — | ||
| Magnetic Field | — | ||
| RA2000 | 07:49:40.0 | ||
| Dec2000 | -52:07:14 | ||
| Alternate Names | |||
| Planetary system | 1 planet |
Related publications
KELT: The Kilodegree Extremely Little Telescope, a Survey for Exoplanets Transiting Bright, Hot Stars
2018
PEPPER J., STASSUN K. & GAUDI S.
in the 'Handbook of Exoplanets,' Springer
arxiv
Ephemeris refinement of 21 Hot Jupiter exoplanets with high timing uncertainties
2018
MALLONN M., von ESSEN C., HERRERO E., ALEXOUDI X., GRANZE T. et al.
Astron. & Astrophys., accepted
arxiv
KELT-14b and KELT-15b: An Independent Discovery of WASP-122b and a New Hot Jupiter
2016
RODRIGUEZ J., COLON K., STASSUN K., WRIGHT D., CRGILE Ph. et al.
Astron. J., submitted
paper arxiv ADS
