Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Lyra [1] |
Kepler-13 A | |
Right ascension | 19h 07m 53.1397s [2] |
Declination | 46° 52′ 05.922″ [2] |
Apparent magnitude (V) | 9.95 [3] |
Kepler-13 B | |
Right ascension | 19h 07m 53.0281s [4] |
Declination | 46° 52′ 06.126″ [4] |
Apparent magnitude (V) | 10.33 [5] |
Characteristics | |
Spectral type | A0 |
Variable type | Planetary transit variable [6] |
Astrometry | |
Kepler-13 A | |
Proper motion (μ) | RA: −4.411(42) mas/yr [2] Dec.: −15.220(50) mas/yr [2] |
Parallax (π) | 2.0319 ± 0.0344 mas [2] |
Distance | 1,610 ± 30 ly (492 ± 8 pc) |
Kepler-13 B | |
Proper motion (μ) | RA: −4.060(33) mas/yr [4] Dec.: −15.512(40) mas/yr [4] |
Parallax (π) | 2.0912 ± 0.0263 mas [4] |
Distance | 1,560 ± 20 ly (478 ± 6 pc) |
Details [7] | |
Kepler-13A | |
Mass | 1.72±0.10 M☉ |
Radius | 1.71±0.04 R☉ |
Surface gravity (log g) | 4.2±0.5 cgs |
Temperature | 7650±250 K |
Metallicity [Fe/H] | 0.2±0.2 dex |
Rotational velocity (v sin i) | 78±15 km/s |
Age | 0.5±0.1 Gyr |
Kepler-13B | |
Mass | 1.68±0.10 M☉ |
Radius | 1.68±0.04 R☉ |
Surface gravity (log g) | 4.2±0.5 cgs |
Temperature | 7530±250 K |
Metallicity [Fe/H] | 0.2±0.2 dex |
Rotational velocity (v sin i) | 69±13 km/s |
Age | 0.5±0.1 Gyr |
Other designations | |
Database references | |
SIMBAD | data |
Kepler-13 or KOI-13 is a stellar triple star system consisting of Kepler-13A, around which an orbiting hot Jupiter exoplanet was discovered with the Kepler spacecraft in 2011, and Kepler-13B a common proper motion companion star which has an additional star orbiting it. [8]
The multiple nature of the system was discovered in 1904 by Robert Grant Aitken at Lick Observatory. He measured a separation between the A and B components of approximately one arc second and position angle of 281.3° with the 36" James Lick telescope. [9] The position of the two visual components of the system relative to each other has remained constant since 1904. [10] Radial velocity measurements taken with the SOPHIE échelle spectrograph at the Haute-Provence Observatory revealed an additional companion orbiting Kepler-13B. This companion has a mass of between 0.4 and 1 times that of the Sun and orbits with a period of 65.831 days with an eccentricity of 0.52 [8]
Kepler-13 was identified as one of 1235 planetary candidates with transit-like signatures in the first four months of Kepler data. [11] It was confirmed as a planet by measuring the Doppler beaming effect on the Kepler light curve. [6] The planet that has been confirmed, having a radius of between 1.5 and 2.6 RJ, is also one of the largest known exoplanets.
The planet is likely to be tidally locked to the parent star. In 2015, the planetary nightside temperature was estimated to be equal to 2394±251 K. [12]
The study in 2012, utilizing a Rossiter–McLaughlin effect, have determined the planetary orbit is mildly misaligned with the equatorial plane of the star, misalignment equal to 24±4°. [13]
The planetary transits are changing in duration over time which is likely caused by the interaction of the planet with its host star. [14] [15]
In 2017, it was revealed that titanium monoxide molecules in the dayside might be carried to the nightside of the planet, where they form clouds and precipitate. [16]
Companion (in order from star) | Mass | Semimajor axis (AU) | Orbital period (days) | Eccentricity | Inclination | Radius |
---|---|---|---|---|---|---|
b | 9.28(16) MJ | 0.03641(87) | 1.763588(1) | 0.00064+0.00012 −0.00016 | 86.770+0.048 −0.052 ° | 2.216(87) RJ |
Kepler-4b, initially known as KOI 7.01, is an extrasolar planet first detected as a transit by the Kepler spacecraft. Its radius and mass are similar to that of Neptune; however, due to its proximity to its host star, it is substantially hotter than any planet in the Solar System. The planet's discovery was announced on January 4, 2010, in Washington, D.C., along with four other planets that were initially detected by the Kepler spacecraft and subsequently confirmed by telescopes at the W.M. Keck Observatory.
Kepler-18 is a star with almost the same mass as the Sun in the Cygnus constellation.
Kepler-80, also known as KOI-500, is a red dwarf star of the spectral type M0V. This stellar classification places Kepler-80 among the very common, cool, class M stars that are still within their main evolutionary stage, known as the main sequence. Kepler-80, like other red dwarf stars, is smaller than the Sun, and it has both radius, mass, temperatures, and luminosity lower than that of our own star. Kepler-80 is found approximately 1,223 light years from the Solar System, in the stellar constellation Cygnus, also known as the Swan.
Kepler-68 is a Sun-like main sequence star located 471 light-years away in the constellation Cygnus. It is known to have at least four planets orbiting around it. The third planet has a mass similar to Jupiter but orbits within the habitable zone.
Kepler-32 is an M-type main sequence star located about 1070 light years from Earth, in the constellation of Cygnus. Discovered in January 2012 by the Kepler spacecraft, it shows a 0.58 ± 0.05 solar mass (M☉), a 0.53 ± 0.04 solar radius (R☉), and temperature of 3900.0 K, making it half the mass and radius of the Sun, two-thirds its temperature and 5% its luminosity.
Kepler-69 is a G-type main-sequence star similar to the Sun in the constellation Cygnus, located about 2,430 ly (750 pc) from Earth. On April 18, 2013 it was announced that the star has two planets. Although initial estimates indicated that the terrestrial planet Kepler-69c might be within the star's habitable zone, further analysis showed that the planet very likely is interior to the habitable zone and is far more analogous to Venus than to Earth and thus completely inhospitable.
Kepler-56 is a red giant in constellation Cygnus roughly 3,060 light-years (940 pc) away with slightly more mass than the Sun.
Kepler-25 is a star in the northern constellation of Lyra. It is slightly larger and more massive than the Sun, with a luminosity 21⁄2 times that of the Sun. With an apparent visual magnitude of 10.6, this star is too faint to be seen with the naked eye.
Kepler-102 is a star 353 light-years away in the constellation of Lyra. Kepler-102 is less luminous than the Sun. The star system does not contain any observable amount of dust. Kepler-102 is suspected to be orbited by a binary consisting of two red dwarf stars, at projected separations of 591 and 627 AU.
Kepler-138, also known as KOI-314, is a red dwarf located in the constellation Lyra, 219 light years from Earth. It is located within the field of vision of the Kepler spacecraft, the satellite that NASA's Kepler Mission used to detect planets transiting their stars.
Kepler-30 is a star in the northern constellation of Lyra. It is located at the celestial coordinates: Right Ascension 19h 01m 08.0747s Declination +38° 56′ 50.219″. With an apparent visual magnitude of 15.5, this star is too faint to be seen with the naked eye. Kepler-30 is exhibiting a strong starspot activity.
Kepler-29 is a Sun-like star in the northern constellation of Cygnus. It is located at the celestial coordinates: Right Ascension 19h 53m 23.6020s, Declination +47° 29′ 28.436″. With an apparent visual magnitude of 15.456, this star is too faint to be seen with the naked eye. It is a solar analog, having a close mass, radius, and temperature as the Sun. Currently the age of the star has not been determined due to its 2780 light-year distance. As of 2016 no Jovian exoplanets of 0.9–1.4 MJ have been found at a distance of 5 AU.
Kepler-444 is a triple star system, estimated to be 11.2 billion years old, approximately 119 light-years (36 pc) away from Earth in the constellation Lyra. On 27 January 2015, the Kepler spacecraft is reported to have confirmed the detection of five sub-Earth-sized rocky exoplanets orbiting the main star. The star is a K-type main sequence star. All of the planets are far too close to their star to harbour life forms.
Kepler-296 is a binary star system in the constellation Draco. The primary star appears to be a late K-type main-sequence star, while the secondary is a red dwarf.
KOI-256 is a double star located in the constellation Cygnus approximately 575 light-years (176 pc) from Earth. While observations by the Kepler spacecraft suggested the system contained a gas giant exoplanet orbiting a red dwarf, later studies determined that KOI-256 was a binary system composed of the red dwarf orbiting a white dwarf.
HD 179070, also known as Kepler-21, is a star with a closely orbiting exoplanet in the northern constellation of Lyra. At an apparent visual magnitude of 8.25 this was the brightest star observed by the Kepler spacecraft to host a validated planet until the discovery of an exoplanet orbiting HD 212657 in 2018. This system is located at a distance of 354 light-years from the Sun based on parallax measurements, but is drifting closer with a radial velocity of −18.2 km/s.
Kepler-410 is a binary star system. Its primary star, also known as Kepler-410A, is a F-type subgiant star, orbited by the orange dwarf star Kepler-410B on a wide orbit. The companion star was discovered in 2012.