Kepler-102

Nowadays, Kepler-102 is a topic that has gained great relevance in the _var2 area. Since its inception, Kepler-102 has captured the attention of experts and the general public, generating extensive debate about its implications. In this article, we will explore in depth the different aspects of Kepler-102, analyzing its impact on _var3 and its relevance in today's society. Additionally, we will examine possible solutions and alternatives to address the challenges posed by Kepler-102. Through a comprehensive approach, we will seek to understand the complexity of this issue and its influence in various areas.

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]
Distance352.5 ± 0.4 ly
(108.1 ± 0.1 pc)
Details
Mass0.803±0.021[3] M☉
Radius0.724±0.018[3] R☉
Temperature4909±98[3] K
Metallicity 0.11±0.04[3] dex
Rotation26.572±0.153 d[4]
Age1.1+3.6
−0.5[3] Gyr
Other designations
Gaia DR2 2119583201145735808, KOI-82, KIC 10187017, TYC 3544-1383-1, 2MASS J18455585+4712289
Database references
SIMBADdata

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]

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±0.00049 5.286965(12) <0.100 89.78±0.22° 0.460±0.026 R🜨
c <1.7 M🜨 0.06702±0.00059 7.071392(22) <0.094 89.82±0.15° 0.567±0.028 R🜨
d 3.0±1.3 M🜨 0.08618±0.00076 10.3117670(41) <0.092 89.49±0.11° 1.154±0.058 R🜨
e 4.7±1.8 M🜨 0.1162±0.0010 16.1456994(22) <0.089 89.488±0.051° 2.17±0.11 R🜨
f <4.3 M🜨 0.1656±0.0015 27.453592(60) <0.10 89.320±0.037° 0.861±0.022 R🜨

See also

References

  1. ^ a b c d e 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. ^ a b "KOI-82". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 29 January 2018.
  3. ^ a b c d e f 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. 677. 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