Kepler-84

Last updated
Kepler-84
Observation data
Epoch J2000       Equinox J2000
Constellation Cygnus
Right ascension 01h 37m 40.87964s [1]
Declination +12° 04′ 42.1742″ [1]
Characteristics
Spectral type G3 [2]
Astrometry
Proper motion (μ)RA: −0.150  mas/yr
Dec.: −2.872  mas/yr
Parallax (π)0.6929 ± 0.7043  mas
Details
Mass 1 [2]   M☉
Radius 1.2  R☉
Temperature 5,755 [3]   K
Metallicity [Fe/H]+0.09 ± 0.04 [2]   dex
Age 4.9 [4]   Gyr
Other designations
Kepler-84, KOI-1589, Gaia DR2 2073776859551124992, KIC 5301750, 2MASS J19530049+4029458 [1]
Database references
SIMBAD data
ARICNS data

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. [5] 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. [6] Another (which is a background star with a probability 0.5%) is a yellow star of mass 0.855M☉ on projected separations of 0.18±0.05″ or 0.26″ (213.6 AU). [7]

Planetary system

Kepler-84 is orbited by five known planets, four small gas giants and a Super-Earth. Planets Kepler-84b and Kepler-84c were confirmed in 2012 [8] while the rest was confirmed in 2014. [9] To keep the known planetary system stable, no additional giant planets can be located within 7.4 AU from the parent stars. [10]

The Kepler-84 planetary system [11] [12] [13] [14]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b0.126±0.038  MJ 0.0838.725854±0.00006088.24° 0.174±0.045  RJ
c0.064±0.037  MJ 0.10812.882525±0.000093088.24° 0.184±0.047  RJ
d—0.0524.224537±0.000042——0.123±0.024  RJ
e—0.18127.434389±0.000224——0.232±0.044  RJ
f—0.2544.552169±0.000812——0.196±0.038  RJ

Related Research Articles

<span class="mw-page-title-main">Exomoon</span> Moon beyond the Solar System

An exomoon or extrasolar moon is a natural satellite that orbits an exoplanet or other non-stellar extrasolar body.

HD 102195 is an orange-hued star in the zodiac constellation of Virgo with a confirmed exoplanet companion. With an apparent visual magnitude of 8.07, the star is too faint to be seen with the naked eye. The distance to HD 102195 can be estimated from its annual parallax shift of 34.06 mas, yielding a separation of 95.8 light years. It is moving further away from the Earth with a heliocentric radial velocity of 1.85 km/s. This is a high proper motion star and a possible member of the η Cha stellar kinematic group.

Kepler-20 is a star 929 light-years from Earth in the constellation Lyra with a system of 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-33 is a star in the constellation of Cygnus with a system of five known planets. Having just begun to evolve off from the main sequence, its radius and mass are difficult to ascertain, although data available in 2020 shows its best-fit mass of 1.3M☉ and diameter of 1.6R☉ are compatible with a model of a subgiant star.

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 1,218 light years from the Solar System, in the stellar constellation Cygnus, also known as the Swan.

Kepler-102 is a star 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-1625 is a 14th-magnitude solar-mass star located in the constellation of Cygnus approximately 8,000 light years away. Its mass is within 5% of that of the Sun, but its radius is approximately 70% larger reflecting its more evolved state. A candidate gas giant exoplanet was detected by the Kepler Mission around the star in 2015, which was later validated as a likely real planet to >99% confidence in 2016. In 2018, the Hunt for Exomoons with Kepler project reported that this exoplanet has evidence for a Neptune-sized exomoon around it, based on observations from NASA’s Kepler Mission. Subsequent observations by the larger Hubble Space Telescope provided compounding evidence for a Neptune-sized satellite, with an on-going debate about the reality of this exomoon candidate.

KOI-5 is a triple star system composed of three stars: KOI-5 A, KOI-5 B and KOI-5 C, orbiting 1,870±70 light-years away.

Kepler-411 is a binary star system. Its primary star Kepler-411 is a K-type main-sequence star, orbited by the red dwarf star Kepler-411B on a wide orbit, discovered in 2012.

HD 175289 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 "Kepler-84". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved July 13, 2016.
  2. 1 2 3 Vidotto, A. A; Gregory, S. G; Jardine, M; Donati, J. F; Petit, P; Morin, J; Folsom, C. P; Bouvier, J; Cameron, A. C; Hussain, G; Marsden, S; Waite, I. A; Fares, R; Jeffers, S; Do Nascimento, J. D (2014). "Stellar magnetism: Empirical trends with age and rotation" (PDF). Monthly Notices of the Royal Astronomical Society. 441 (3): 2361. arXiv: 1404.2733 . Bibcode:2014MNRAS.441.2361V. doi:10.1093/mnras/stu728. S2CID   43200119.
  3. ↑ Gray, R. O; Corbally, C. J; Garrison, R. F; McFadden, M. T; Robinson, P. E (2003). "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 parsecs: The Northern Sample I". The Astronomical Journal. 126 (4): 2048. arXiv: astro-ph/0308182 . Bibcode:2003AJ....126.2048G. doi:10.1086/378365. S2CID   119417105.
  4. ↑ Melendez, Jorge; Dodds-Eden, Katie; Robles, Jose A (2006). "HD 98618: A Star Closely Resembling our Sun". The Astrophysical Journal. 641 (2): L133–L136. arXiv: astro-ph/0603219 . Bibcode:2006ApJ...641L.133M. doi:10.1086/503898. S2CID   17479387.
  5. ↑ Ramos, X. S.; Charalambous, C.; Benítez-Llambay, P.; Beaugé, C. (2017), "Planetary migration and the origin of the 2:1 and 3:2 (near)-resonant population of close-in exoplanets", Astronomy & Astrophysics, 602: A101, arXiv: 1704.06459 , Bibcode:2017A&A...602A.101R, doi:10.1051/0004-6361/201629642, S2CID   119369796
  6. ↑ Hirsch, Lea A.; Ciardi, David R.; Howard, Andrew W.; Everett, Mark E.; Furlan, Elise; Saylors, Mindy; Horch, Elliott P.; Howell, Steve B.; Teske, Johanna; Marcy, Geoffrey W. (2017), "ASSESSING THE EFFECT OF STELLAR COMPANIONS FROM HIGH-RESOLUTION IMAGING OF Kepler OBJECTS OF INTEREST", The Astronomical Journal, 153 (3): 117, arXiv: 1701.06577 , Bibcode:2017AJ....153..117H, doi:10.3847/1538-3881/153/3/117, S2CID   39321033
  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. ↑ Xie, Ji-Wei (2012), "Transit Timing Variation of Near-Resonance Planetary Pairs: Confirmation of 12 Multiple-Planet Systems", The Astrophysical Journal Supplement Series, 208 (2): 22, arXiv: 1208.3312 , Bibcode:2013ApJS..208...22X, doi:10.1088/0067-0049/208/2/22, S2CID   17160267
  9. ↑ openexoplanetcatalogue.com Kepler-84
  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: 549–563, arXiv: 1702.07714 , Bibcode:2017MNRAS.468..549B, doi:10.1093/mnras/stx461, S2CID   119325005
  11. ↑ Furlan, E.; Howell, S. B. (2017), "The densities of planets in multiple stellar systems", The Astronomical Journal, 154 (2): 66, arXiv: 1707.01942 , Bibcode:2017AJ....154...66F, doi:10.3847/1538-3881/aa7b70, S2CID   28833730
  12. ↑ Planet Kepler-84 d at exoplanets.eu
  13. ↑ Planet Kepler-84 e at exoplanets.eu
  14. ↑ Planet Kepler-84 f at exoplanets.eu
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