Kepler-46

Last updated
Kepler-46
KOI-872 system.jpg
Artist's conception of the Kepler-46 system showing the two planets. Planet b transits its star, the same method by which it was detected.
Observation data
Epoch J2000       Equinox J2000
Constellation Lyra
Right ascension 19h 17m 04.4929s [1]
Declination 42° 36′ 15.041″ [1]
Characteristics
Apparent magnitude  (J)13.814 [2]
Apparent magnitude  (H)13.436 [2]
Apparent magnitude  (K)13.347 [2]
Astrometry
Proper motion (μ)RA: 3.156±0.046 [1]   mas/yr
Dec.: 0.894±0.053 [1]   mas/yr
Parallax (π)1.2586 ± 0.0277  mas [1]
Distance 2,590 ± 60  ly
(790 ± 20  pc)
Absolute bolometric
magnitude  (Mbol)		5.18 (predicted) [note 1]
Details
Mass 0.902+0.040
−0.038 [3]   M☉
Radius 0.938+0.038
−0.039 [3]   R☉
Temperature 5155±150 [3]   K
Metallicity [Fe/H]0.41±0.10 [3] [note 2]   dex
Rotation 27.859±0.075 days [4]
Age 9.7+3.7
−3.5 [3]   Gyr
Other designations
Gaia DR2  2102700131386216576, KOI-872, KIC  7109675, 2MASS J19170449+4236150 [2]
Database references
SIMBAD data
KIC data

Kepler-46, previously designated KOI-872, is a star located in the constellation Lyra. Observed since 2009 by the Kepler space observatory, it has since been found to possess a planetary system consisting of at least three planets and while it has a similar mass to the Sun (90%) it is significantly older at ten billion years. [3]

Contents

Kepler-46 b (previously KOI-872.01), was the first planet discovered in the system. It was found through detailed analysis of Kepler space observatory data. An additional planet, Kepler-46 c, was discovered by an outside group using Kepler public data through analysis of transit timing variations. While only one additional planet was confirmed by the analysis, the study revealed the potential existence of an unconfirmed planet KOI-872.03 (KOI-872 d). [5] Validation by the multiplicity method confirmed the existence of this planet which was then renamed Kepler-46d.

Planetary system

Planet b is a gas giant planet with a mass slightly less than that of Jupiter. [3] The second planet in the system was among the first to be discovered through the method of transit timing variations, and through its confirmation of KOI-872 c with a 99% confidence level has shown that the method of detection may be used to detect future extrasolar planets and, possibly, extrasolar moons. [6] This second planet exerted a gravitational force on the first planet, orbiting its host star in just 34 days. While this usually occurs on an extremely regular schedule, additional planets within the system can disrupt the time of the transit, and these disruptions can indicate the presence of a planet, even if the disrupting planet does not pass in front of the host star itself. [6]

The data show that Kepler-46 c is an approximately Saturn-mass object with an orbital period of 57 days. [6] As the planet does not itself transit its host star, there is no way of knowing its size (probably a similar size to its sibling). The measurements also suggest the existence of another planet orbiting with a period of about 6.8 days, [5] and this planet was confirmed in 2016. [7]

The method in which the planet was detected is similar to the way that the planet Neptune was discovered, in which the newly discovered planet is detected by its pull on another which is already known to exist. [8]

In 2021, it was found the orbital plane of Kepler-46b is slowly changing, likely under the gravitational influence of the additional giant planet. [9]

The Kepler-46 planetary system [5] [3]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
d3.339  M🜨 0.0679±0.00356.76671+0.00013
−0.00012		0(assumed)88.55+0.49
−0.69 ° 		0.1510+0.0094
−0.0098  RJ
b0.885+0.374
−0.343  MJ 		0.1971±0.000133.648+0.004
−0.005		0.0321+0.0069
−0.0078		89.04±0.14 ° 0.810+0.035
−0.36  RJ
c0.362±0.016  MJ 0.2811±0.000357.325+0.116
−0.098		0.0354+0.0057
−0.0059		88.66+0.26
−0.27 ° 		—

Related Research Articles

<span class="mw-page-title-main">Kepler-9</span> Star located in the constellation Lyra

Kepler-9 is a sunlike star in the constellation Lyra. Its planetary system, discovered by the Kepler Mission in 2010 was the first detected with the transit method found to contain multiple planets.

Kepler-17 is a main-sequence yellow dwarf star that is much more active than the Sun with starspots covering roughly 6% of its surface. Starspots are long-lived, with at least one persisting for 1400 days.

Kepler-39 is an F-type main sequence star located in the constellation Cygnus. It is located about 3,560 light-years away. One known substellar companion orbits it, Kepler-39b.

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-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-89 is a star with four confirmed planets. Kepler-89 is a possible wide binary star.

Kepler-65 is a subgiant star slightly more massive than the Sun and has at least four planets.

Kepler-88 is a G-type star 1,230 light-years away in the constellation of Lyra, with three confirmed exoplanets. SIMBAD lists a subgiant spectral type of G8IV, while other sources give it a main sequence spectral type of G6V. The latter is more consistent with its properties.

Kepler-24 is a star in the northern constellation of Lyra. It is located at the celestial coordinates: Right Ascension 19h 21m 39.0s, Declination +38° 20′ 37″. With an apparent visual magnitude of 15.5, this star is too faint to be seen with the naked eye.

<span class="mw-page-title-main">Kepler-25</span> Yellow-white hued star in the constellation Lyra

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.

<span class="mw-page-title-main">Kepler-26</span> Star in the constellation Lyra

Kepler-26 is a star in the northern constellation of Lyra. It is located at the celestial coordinates: Right Ascension 18h 59m 45.8407s Declination +46° 33′ 59.438″. With an apparent visual magnitude of 15.5, 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-61 is a K-type main-sequence star approximately 1,100 light years from Earth in the constellation Cygnus. It is located within the field of vision of the Kepler spacecraft, the satellite that NASA's Kepler Mission used to detect planets that may be transiting their stars. On April 24, 2013 it was announced that the star has an extrasolar planet orbiting in the inner edge of the habitable zone, named Kepler-61b.

<span class="mw-page-title-main">Kepler-138</span> Red dwarf in the constellation Lyra

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-28 is a star in the northern constellation of Cygnus., It is orbited by two exoplanets. It is located at the celestial coordinates: Right Ascension 19h 28m 32.8905s, Declination +42° 25′ 45.959″. With an apparent visual magnitude of 15.036, this star is too faint to be seen with the naked eye.

Kepler-43, formerly known as KOI-135, is a star in the northern constellation of Cygnus. It is located at the celestial coordinates: Right Ascension 19h 00m 57.8034s, Declination +46° 40′ 05.665″. With an apparent visual magnitude of 13.996, this star is too faint to be seen with the naked eye. The Kepler-43 has a very strong starspot activity.

Kepler-419 is an F-type main-sequence star located about 3,400 light years from Earth in the constellation Cygnus. It is located within the field of vision of the Kepler spacecraft, the satellite that NASA's Kepler Mission used to detect planets that may be transiting their stars. In 2012, a potential planetary companion in a very eccentric orbit was detected around this star, but its planetary nature was not confirmed until 12 June 2014, when it was named Kepler-419b. A second planet was announced orbiting further out from the star in the same paper, named Kepler-419c.

References

  1. 1 2 3 4 5 Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics . 616. A1. arXiv: 1804.09365 . Bibcode: 2018A&A...616A...1G . doi: 10.1051/0004-6361/201833051 . Gaia DR2 record for this source at VizieR.
  2. 1 2 3 4 "Kepler-46". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved May 16, 2012.
  3. 1 2 3 4 5 6 7 8 Saad-Olivera, Ximena; et al. (2017). "Masses of Kepler-46b, c from Transit Timing Variations". The Astronomical Journal. 153 (4). 198. arXiv: 1704.01541 . Bibcode:2017AJ....153..198S. doi: 10.3847/1538-3881/aa64e0 . S2CID   119513521.
  4. ↑ McQuillan, A.; Mazeh, T.; Aigrain, S. (2013). "Stellar Rotation Periods of The Kepler objects of Interest: A Dearth of Close-In Planets Around Fast Rotators". The Astrophysical Journal Letters. 775 (1). L11. arXiv: 1308.1845 . Bibcode:2013ApJ...775L..11M. doi:10.1088/2041-8205/775/1/L11. S2CID   118557681.
  5. 1 2 3 Nesvorny, D.; et al. (2012). "The Detection and Characterization of a Nontransiting Planet by Transit Timing Variations". Science. 336 (6085): 1133–6. arXiv: 1208.0942 . Bibcode:2012Sci...336.1133N. doi:10.1126/science.1221141. PMID   22582018. S2CID   41455466.
  6. 1 2 3 Moskowitz, Clara (May 10, 2012). "Hidden Alien Planet Revealed by Its Own Gravity". Space.com. Space.com. Retrieved May 10, 2012.
  7. ↑ Huang, Chelsea; Wu, Yanqin; Triaud, Amaury H. M. J. (2016), "Warm Jupiters Are Less Lonely Than Hot Jupiters: Close Neighbors", The Astrophysical Journal, 825 (2): 98, arXiv: 1601.05095 , Bibcode:2016ApJ...825...98H, doi: 10.3847/0004-637X/825/2/98 , S2CID   119290761
  8. ↑ Crockett, Christopher (May 12, 2012). "New planet found in distant solar system by its tug on another world". EarthSky. Earthsky Communications. Retrieved May 19, 2012.
  9. ↑ Shahaf, Sahar; Mazeh, Tsevi; Zucker, Shay; Fabrycky, Daniel (2021), "Systematic search for long-term transit duration changes in Kepler transiting planets", Monthly Notices of the Royal Astronomical Society, 505 (1): 1293–1310, arXiv: 2105.04318 , Bibcode:2021MNRAS.505.1293S, doi:10.1093/mnras/stab1359

Notes

  1. ↑ Figure based on the following equations, which calculated bolometric (total) luminosity across all spectra based on effective temperature: (cf. Luminosity) and (cf. Absolute magnitude)
  2. ↑ This measurement indicates the log10 of the relative abundance of iron in the measured star to that of the Sun.
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.