Kepler-102

Last updated
Kepler-102
Observation data
Epoch J2000       Equinox J2000
Constellation Lyra
Right ascension 18h 45m 55.85599s [1]
Declination +47° 12′ 28.8453″ [1]
Apparent magnitude  (V)12.07 [2]
Characteristics
Spectral type K3V [2]
Astrometry
Radial velocity (Rv)−28.51±0.37 [1]  km/s
Proper motion (μ)RA: −41.044  mas/yr [1]
Dec.: −43.267  mas/yr [1]
Parallax (π)9.2517 ± 0.0102  mas [1]
Distance 352.5 ± 0.4  ly
(108.1 ± 0.1  pc)
Details
Mass 0.803±0.021 [3]   M☉
Radius 0.724±0.018 [3]   R☉
Temperature 4909±98 [3]   K
Metallicity [Fe/H]0.11±0.04 [3]   dex
Rotation 26.572±0.153 d [4]
Age 1.1+3.6
−0.5 [3]   Gyr
Other designations
Gaia DR2  2119583201145735808, KOI-82, KIC  10187017, TYC  3544-1383-1, 2MASS J18455585+4712289
Database references
SIMBAD data

Kepler-102 is a star 353 light-years (108 parsecs ) away in the constellation of Lyra. Kepler-102 is less luminous than the Sun. [5] The star system does not contain any observable amount of dust. [6] Kepler-102 is suspected to be orbited by a binary consisting of two red dwarf stars, at projected separations of 591 and 627 AU. [7]

Contents

Planetary system

In January 2014, a system of five planets around the star was announced, three of them being smaller than Earth. While 3 of the transit signals were discovered during the first year of the Kepler mission, their small size made them hard to confirm as possibilities of these being false positives were needed to be removed. Later, two other signals were detected. Follow-up radial velocity data helped to determine the mass of the two largest planets (Kepler-102d and Kepler-102e). [8]

By 2017, the search for additional planets utilizing the transit-timing variation method had yielded zero results, [9] although the presence of planets with semimajor axis beyond 10 AU cannot be excluded. [10]

The Kepler-102 planetary system [3]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b<1.1  M🜨 0.05521±0.000495.286965(12)<0.10089.78±0.22 ° 0.460±0.026  R🜨
c<1.7  M🜨 0.06702±0.000597.071392(22)<0.09489.82±0.15 ° 0.567±0.028  R🜨
d3.0±1.3  M🜨 0.08618±0.0007610.3117670(41)<0.09289.49±0.11 ° 1.154±0.058  R🜨
e4.7±1.8  M🜨 0.1162±0.001016.1456994(22)<0.08989.488±0.051 ° 2.17±0.11  R🜨
f<4.3  M🜨 0.1656±0.001527.453592(60)<0.1089.320±0.037 ° 0.861±0.022  R🜨

See also

Related Research Articles

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 3,500 light-years away. One known substellar companion orbits it, Kepler-39b.

Kepler-19 is a G7V star that is host to three known planets - Kepler-19b, Kepler-19c, and Kepler-19d. It is located about 720 light-years away in the constellation Lyra, five arcminutes northwest of the much more distant open cluster NGC 6791.

Kepler-20 is a star about 934 light-years from Earth in the constellation Lyra with a system of at least five, and possibly six, known planets. The apparent magnitude of this star is 12.51, so it cannot be seen with the unaided eye. Viewing it requires a telescope with an aperture of 15 cm (6 in) or more. It is slightly smaller than the Sun, with 94% of the Sun's radius and about 91% of the Sun's mass. The effective temperature of the photosphere is slightly cooler than that of the Sun at 5466 K, giving it the characteristic yellow hue of a stellar class G8 star. The abundance of elements other than hydrogen or helium, what astronomers term the metallicity, is approximately the same as in the Sun. It may be older than the Sun, although the margin of error here is relatively large.

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 1053 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-65 is a subgiant star slightly more massive than the Sun and has at least four planets.

Kepler-66 is a star with slightly more mass than the Sun in the NGC 6811 open cluster in the Cygnus constellation. It has one confirmed planet, slightly smaller than Neptune, announced in 2013.

Kepler-67 is a star in the open cluster NGC 6811 in the constellation Cygnus. It has slightly less mass than the Sun and has one confirmed planet, slightly smaller than Neptune, announced in 2013.

<span class="mw-page-title-main">Kepler-56</span> Red giant star in the constellation Cygnus

Kepler-56 is a red giant in constellation Cygnus roughly 3,030 light-years (930 pc) away with slightly more mass than the Sun.

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.

<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 45.8408s 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.

<span class="mw-page-title-main">Kepler-444</span> Triple star system in the constellation of Lyra

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-107 is a star about 1,694 light-years away in the constellation Cygnus. It is a spectral type G2 star. An imaging survey in 2016 failed to find any stellar companions to it.

<span class="mw-page-title-main">HD 179070</span> Star in the constellation Lyra

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.

References

  1. 1 2 3 4 5 6 Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv: 2208.00211 . Bibcode:2023A&A...674A...1G. doi: 10.1051/0004-6361/202243940 . S2CID   244398875. Gaia DR3 record for this source at VizieR.
  2. 1 2 "KOI-82". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 29 January 2018.
  3. 1 2 3 4 5 6 Bonomo, A. S.; Dumusque, X.; et al. (April 2023). "Cold Jupiters and improved masses in 38 Kepler and K2 small-planet systems from 3661 high-precision HARPS-N radial velocities. No excess of cold Jupiters in small-planet systems". Astronomy & Astrophysics . arXiv: 2304.05773 . Bibcode:2023A&A...677A..33B. doi:10.1051/0004-6361/202346211. S2CID   258078829.
  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. ↑ "Kepler-102". NASA Exoplanet Archive . Retrieved 21 April 2023.
  6. ↑ Dusty phenomena in the vicinity of giant exoplanets
  7. ↑ Kraus, Adam L.; Ireland, Michael J.; Huber, Daniel; Mann, Andrew W.; Dupuy, Trent J. (2016), "The Impact of Stellar Multiplicity on Planetary Systems. I. The Ruinous Influence of Close Binary Companions", The Astronomical Journal, 152 (1): 8, arXiv: 1604.05744 , Bibcode:2016AJ....152....8K, doi: 10.3847/0004-6256/152/1/8 , S2CID   119110229
  8. ↑ Masses, radii, and orbits of small Kepler planets: the transition from gaseous to rocky planets accessdate=8 January 2014
  9. ↑ Schmitt, Joseph R.; Jenkins, Jon M.; Fischer, Debra A. (2017), "A SEARCH FOR LOST PLANETS IN THE KEPLER MULTI-PLANET SYSTEMS AND THE DISCOVERY OF THE LONG-PERIOD, NEPTUNE-SIZED EXOPLANET KEPLER-150 f", The Astronomical Journal, 153 (4): 180, arXiv: 1703.09229 , Bibcode:2017AJ....153..180S, doi: 10.3847/1538-3881/aa62ad , PMC   5783551 , PMID   29375142
  10. ↑ Becker, Juliette C.; Adams, Fred C. (2017), "Effects of Unseen Additional Planetary Perturbers on Compact Extrasolar Planetary Systems", Monthly Notices of the Royal Astronomical Society, 468 (1): 549–563, arXiv: 1702.07714 , Bibcode:2017MNRAS.468..549B, doi:10.1093/mnras/stx461, S2CID   119325005
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