HD 187123 is a single,[7] yellow-hued star with two exoplanetary companions in the northern constellation of Cygnus. It has an apparent visual magnitude of 7.83,[2] making it an 8th magnitude star that is too faint to be visible with the naked eye. However, it should be easy _target with binoculars or small telescope. The system is located at a distance of 150 light years from the Sun based on parallax measurements, but is drifting closer with a radial velocity of −17 km/s.[1]

HD 187123

HD 187123 has a planetary system with at least two planets in it. Artist's rendition of planets HD 187123 b and c.
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Cygnus
Right ascension 19h 46m 58.1122s[1]
Declination +34° 25′ 10.281″[1]
Apparent magnitude (V) 7.83[2]
Characteristics
Spectral type G2V[3]
B−V color index 0.661±0.010[2]
Astrometry
Radial velocity (Rv)−16.91(12)[1] km/s
Proper motion (μ) RA: 142.591(15) mas/yr[1]
Dec.: −123.715(18) mas/yr[1]
Parallax (π)21.7166 ± 0.0157 mas[1]
Distance150.2 ± 0.1 ly
(46.05 ± 0.03 pc)
Absolute magnitude (MV)4.41[2]
Details
Mass1.06±0.02[4] M
Radius1.17±0.03[4] R
Luminosity1.44±0.02[4] L
Surface gravity (log g)4.32±0.03[4] cgs
Temperature5,853±53[4] K
Metallicity [Fe/H]0.121±0.030[5] dex
Rotational velocity (v sin i)2.15±0.50[5] km/s
Age5.6±1.3[4] Gyr
Other designations
BD+34°3708, HD 187123, HIP 97336, SAO 68845, LTT 15779[6]
Database references
SIMBADdata

This is an ordinary G-type main-sequence star with a stellar classification of G2V.[3] The physical properties of this star are sufficiently similar to the Sun that it has been considered a solar analog, although the metallicity is higher.[8] It is estimated to be five or six billion years old and is spinning with a projected rotational velocity of 2 km/s.[5] The star has a similar mass to the Sun but is slightly larger with 117% of the Sun's radius. It is radiating 1.44 times the luminosity of the Sun from its photosphere at an effective temperature of 5,853 K.[4]

Planetary system

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In 1998 the California and Carnegie Planet Search team, after following a suggestion by Kevin Apps, a Briton who at the time was an undergraduate student[9] found a possible planet orbiting the star.[10] There were also indications of another, more distant body orbiting the star and this claim was published in 2006.[11] This planet was confirmed in 2009.[12] The presence of water has been detected in the atmosphere of HD 187123 b with high confidence.[13]

The HD 187123 planetary system[5]
Companion
(in order from star)
Mass Semimajor axis
(AU)
Orbital period
(days)
Eccentricity Inclination Radius
b >0.5074±0.0026 MJ 0.04213±0.00034 3.0965886±0.0000043 0.0093±0.0046
c >1.818±0.035 MJ 4.417±0.054 3324±46 0.280±0.022

See also

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References

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  1. ^ a b c d e f 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 c d 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. ^ a b Gray, R. O.; et al. (2001). "The Physical Basis of Luminosity Classification in the Late A-, F-, and Early G-Type Stars. I. Precise Spectral Types for 372 Stars". The Astronomical Journal. 121 (4): 2148. Bibcode:2001AJ....121.2148G. doi:10.1086/319956. S2CID 117076031.
  4. ^ a b c d e f g 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. ^ a b c d Feng, Y. Katherina; et al. (2015). "The California Planet Survey IV: A Planet Orbiting the Giant Star HD 145934 and Updates to Seven Systems with Long-period Planets". The Astrophysical Journal. 800 (1). 22. arXiv:1501.00633. Bibcode:2015ApJ...800...22F. doi:10.1088/0004-637X/800/1/22. S2CID 56390823.
  6. ^ "HD 187123". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2021-10-14.
  7. ^ Ginski, C.; et al. (April 2012). "A lucky imaging multiplicity study of exoplanet host stars". Monthly Notices of the Royal Astronomical Society. 421 (3): 2498–2509. arXiv:1202.4586. Bibcode:2012MNRAS.421.2498G. doi:10.1111/j.1365-2966.2012.20485.x.
  8. ^ Soubiran, C.; Triaud, A. (May 2004). "The Top Ten solar analogs in the ELODIE library". Astronomy and Astrophysics. 418 (3): 1089–1100. arXiv:astro-ph/0402094. Bibcode:2004A&A...418.1089S. doi:10.1051/0004-6361:20035708.
  9. ^ "British student shows Nasa new planet". BBC News. September 25, 1998. Retrieved December 31, 2011.
  10. ^ Butler, R. Paul; et al. (1998). "A Planet with a 3.1 Day Period around a Solar Twin". Publications of the Astronomical Society of the Pacific. 110 (754): 1389–1393. Bibcode:1998PASP..110.1389B. CiteSeerX 10.1.1.37.5463. doi:10.1086/316287. S2CID 16360564.
  11. ^ Wright, J. T.; et al. (2007). "Four New Exoplanets and Hints of Additional Substellar Companions to Exoplanet Host Stars". The Astrophysical Journal. 657 (1): 533–545. arXiv:astro-ph/0611658. Bibcode:2007ApJ...657..533W. doi:10.1086/510553. S2CID 35682784.
  12. ^ Wright, J. T.; et al. (2009). "Ten New and Updated Multi-planet Systems, and a Survey of Exoplanetary Systems". The Astrophysical Journal. 693 (2): 1084–1099. arXiv:0812.1582. Bibcode:2009ApJ...693.1084W. doi:10.1088/0004-637X/693/2/1084. S2CID 18169921.
  13. ^ Buzard, Cam; et al. (July 2020). "Simulating the Multi-epoch Direct Detection Technique to Isolate the Thermal Emission of the Non-transiting Hot Jupiter HD187123b". The Astronomical Journal. 160 (1): 13. arXiv:2005.03020. Bibcode:2020AJ....160....1B. doi:10.3847/1538-3881/ab8f9c. S2CID 218538482. 1.
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