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BD+14 4559

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Orange-hued star in the constellation Pegasus Not to be confused with the Polaris star.
BD+14 4559 / Solaris
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Pegasus
Right ascension 21 13 35.9901
Declination +14° 41′ 21.7846″
Apparent magnitude (V) 9.78
Characteristics
Spectral type K2V
B−V color index 1.611±0.218
V−R color index 0.68
R−I color index 0.50
Astrometry
Radial velocity (Rv)−44.30±0.30 km/s
Proper motion (μ) RA: 233.993±0.057 mas/yr
Dec.: −0.275±0.056 mas/yr
Parallax (π)20.2337 ± 0.0345 mas
Distance161.2 ± 0.3 ly
(49.42 ± 0.08 pc)
Absolute magnitude (MV)6.14
Absolute bolometric
magnitude
 (Mbol)
5.56
Details
Mass0.82±0.02 M
Radius0.78±0.02 R
Luminosity0.32±0.01 L
Luminosity (bolometric)0.4786 L
Surface gravity (log g)4.57±0.03 cgs
Temperature4,948±25 K
Metallicity 0.10±0.07 dex
Age6.9±4.2 Gyr
Other designations
Solaris, AG+14 2370, BD+14 4559, HIP 104780, PPM 139779, LTT 16221
Database references
SIMBADdata
Exoplanet Archivedata

BD+14 4559 is a star with an exoplanetary companion in the northern constellation of Pegasus. During the 2019 NameExoWorlds campaign, the star was named Solaris by Poland after a 1961 science fiction novel about an ocean-covered exoplanet by Polish writer Stanisław Lem. With an apparent visual magnitude of 9.78, the star is too faint to be viewed with the naked eye. The system is located at a distance of 161 light-years from the Sun based on parallax measurements, but is drifting closer with a radial velocity of −44 km/s. It is a high proper motion star, traversing the celestial sphere at an angular rate of 0.234″ yr.

This is an ordinary K-type main sequence star with a stellar classification of K2V. The age of the star is poorly constrained, but is estimated to be roughly seven billion years. It has 82% of the mass and 78% of the radius of the Sun. The star is radiating 48% of the net luminosity of the Sun from its photosphere at an effective temperature of 4,948 K. It has a higher metallicity – the abundance of elements of higher atomic number than helium – compared to the Sun.

Planetary system

On June 10, 2009, an exoplanet (Pirx) was found in orbit by Niedzielski et al. using the Hobby-Eberly Telescope. It has a minimum mass of one and a half Jupiter masses (MJ). The orbit of this object is highly eccentric and it spends 65% of its orbital period in the star's habitable zone. A 2020 analysis of data from the Gaia mission has set a 3-sigma upper limit to its mass of 49.83 MJ. There may be an undetected second planet orbiting the star, however this is unconfirmed.

The BD+14 4559 planetary system
Companion
(in order from star)
Mass Semimajor axis
(AU)
Orbital period
(days)
Eccentricity Inclination Radius
b / Pirx >1.52 ± 0.19 MJ 0.777 268.94 ± 0.99 0.29 ± 0.03 >1.769°
c (unconfirmed) >2.4 MJ >2.3 800?

See also

References

  1. ^ 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. ^ Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. S2CID 119257644.
  3. ^ Niedzielski, A.; et al. (2009). "Substellar-mass Companions to the K-dwarf BD+14 4559 and the K-giants HD 240210 and BD+20 2457". The Astrophysical Journal. 707 (1): 768–777. arXiv:0906.1804. Bibcode:2009ApJ...707..768N. doi:10.1088/0004-637X/707/1/768. S2CID 16877069.
  4. ^ Bonfanti, A.; et al. (2016). "Age consistency between exoplanet hosts and field stars". Astronomy & Astrophysics. 585: 14. arXiv:1511.01744. Bibcode:2016A&A...585A...5B. doi:10.1051/0004-6361/201527297. S2CID 53971692. A5.
  5. "9 Cet". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2021-11-12.
  6. "Approved names". NameExoworlds. Retrieved 2020-01-02.
  7. Lépine, Sébastien; Shara, Michael M. (March 2005). "A Catalog of Northern Stars with Annual Proper Motions Larger than 0.15" (LSPM-NORTH Catalog)". The Astronomical Journal. 129 (3): 1483–1522. arXiv:astro-ph/0412070. Bibcode:2005AJ....129.1483L. doi:10.1086/427854. S2CID 2603568.
  8. Hinkel, Natalie R.; Kane, Stephen R. (September 2013). "Habitability of Exomoons at the Hill or Tidal Locking Radius". The Astrophysical Journal. 774 (1): 10. arXiv:1307.4760. Bibcode:2013ApJ...774...27H. doi:10.1088/0004-637X/774/1/27. S2CID 5072506. 27.
  9. ^ Kiefer, F.; et al. (2021). "Determining the true mass of radial-velocity exoplanets with Gaia". Astronomy & Astrophysics. 645: A7. arXiv:2009.14164. Bibcode:2021A&A...645A...7K. doi:10.1051/0004-6361/202039168. S2CID 221995447.
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