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

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

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

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Kepler-84 is a Sun-like star 4,700 light-years from the Sun. It is a G-type star. The stellar radius measurement has a large uncertainty of 48% as in 2017, complicating the modelling of the star. The Kepler-84 star has two suspected stellar companions. Four red dwarfs are few arcseconds away and at least one is probably gravitationally bound to Kepler-84. Another is a yellow star of mass 0.855M☉ on projected separations of 0.18±0.05″ or 0.26″.

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References

  1. 1 2 3 4 5 6 Vallenari, A.; et al. (Gaia Collaboration) (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics . arXiv: 2208.00211 . doi: 10.1051/0004-6361/202243940 . 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 .
  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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