HD 50554

HD 50554
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Gemini
Right ascension 06h 54m 42.82615s[1]
Declination +24° 14′ 44.0057″[1]
Apparent magnitude (V) +6.84[2]
Characteristics
Spectral type F8V[3]
B−V color index 0.582±0.008[2]
Astrometry
Radial velocity (Rv)−3.77±0.13[1] km/s
Proper motion (μ) RA: −35.839 mas/yr[1]
Dec.: −96.668 mas/yr[1]
Parallax (π)32.1855 ± 0.0242 mas[1]
Distance101.34 ± 0.08 ly
(31.07 ± 0.02 pc)
Absolute magnitude (MV)4.46[2]
Details
Mass1.06±0.03[4] M☉
Radius1.07±0.03[4] R☉
Luminosity1.37±0.01[4] L☉
Surface gravity (log g)4.4±0.04[4] cgs
Temperature6,036±52[4] K
Metallicity [Fe/H]0.05±0.06[5] dex
Rotational velocity (v sin i)2.3[5] km/s
Age3.3±1.4 Gyr[4]
2.1±1.6[5] Gyr
Other designations
BD+24°1451, GC 9043, HD 50554, HIP 33212, SAO 78855, GSC 01894-01961[6]
Database references
SIMBADdata

HD 50554 is a single,[7] Sun-like[8] star with an exoplanetary companion in the northern constellation of Gemini. It has an apparent visual magnitude of +6.84,[2] which makes it a 7th magnitude star; it is not visible to the naked eye, but can be viewed with binoculars or a telescope. The system is located at a distance of 101 light-years (31 parsecs) from the Sun based on parallax, but is drifting closer with a radial velocity of −4 km/s.[1]

This is a yellow-white hued F-type main-sequence star with a stellar classification of F8V.[3] Age estimates put it at around 2–3 billion years old. It has a Sun-like metallicity a low level of chromospheric activity[9] and is spinning with a projected rotational velocity of 2.3 km/s.[5] The star has a slightly higher mass and larger radius than the Sun. It is radiating 137% of the luminosity of the Sun from its photosphere at an effective temperature of 6,036 K.[4]

Planetary system

In 2001, a giant planet was announced by the European Southern Observatory, who used the radial velocity method.[10][9] The discovery was formally published in 2002 using observations from the Lick and Keck telescopes.[3] In 2023, the inclination and true mass of HD 50554 b were determined via astrometry.[11]

An infrared excess indicates a debris disk is orbiting the star at a distance of 45 AU with a half-width of 4 AU. This may be an analog of the Kuiper belt at an earlier stage of its evolution, which suggests a Neptune-like planet could be orbiting at its inner edge.[8]

The HD 50554 planetary system[11][8]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(years) 		Eccentricity Inclination Radius
b 5.85+0.9
−0.52 MJ 		2.339+0.03
−0.029 		3.39+0.02
−0.023 		0.482+0.015
−0.015 		61±12 or 119±12° —
Disk 45 AU — —

See also

References

  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 c Fischer, Debra A.; et al. (2002). "Planetary Companions to HD 136118, HD 50554, and HD 106252". Publications of the Astronomical Society of the Pacific. 114 (795): 529–535. Bibcode:2002PASP..114..529F. doi:10.1086/341677. JSTOR 10.1086/341677.
  4. ^ a b c d e f g Bonfanti, A.; et al. (2015). "Revising the ages of planet-hosting stars". Astronomy and Astrophysics. 575. A18. arXiv:1411.4302. Bibcode:2015A&A...575A..18B. doi:10.1051/0004-6361/201424951. S2CID 54555839.
  5. ^ a b c d Chavero, C.; et al. (August 2019). "Emerging trends in metallicity and lithium properties of debris disc stars". Monthly Notices of the Royal Astronomical Society. 487 (3, p.3162-3177): 3162–3177. arXiv:1905.12066. Bibcode:2019MNRAS.487.3162C. doi:10.1093/mnras/stz1496. S2CID 168169634.
  6. ^ "HD 50554". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2021-10-24.
  7. ^ Baines, Ellyn K.; et al. (July 2010). "Ruling Out Possible Secondary Stars to Exoplanet Host Stars Using the CHARA Array". The Astronomical Journal. 140 (1): 167–176. arXiv:1005.2930. Bibcode:2010AJ....140..167B. doi:10.1088/0004-6256/140/1/167. S2CID 14038146.
  8. ^ a b c Dodson-Robinson, Sarah E.; et al. (December 2016). "Herschel Observations and Updated Spectral Energy Distributions of Five Sunlike Stars with Debris Disks". The Astrophysical Journal. 833 (2): 11. arXiv:1610.01173. Bibcode:2016ApJ...833..183D. doi:10.3847/1538-4357/833/2/183. S2CID 118685442. 183.
  9. ^ a b Perrier, C.; et al. (2003). "The ELODIE survey for northern extra-solar planets. I. Six new extra-solar planet candidates". Astronomy and Astrophysics. 410 (3): 1039–1049. arXiv:astro-ph/0308281. Bibcode:2003A&A...410.1039P. doi:10.1051/0004-6361:20031340. S2CID 6946291.
  10. ^ "Exoplanets: The Hunt Continues!" (Press release). Garching, Germany: European Southern Observatory. April 4, 2001. Retrieved December 27, 2012.
  11. ^ a b Xiao, Guang-Yao; Liu, Yu-Juan; et al. (May 2023). "The Masses of a Sample of Radial-Velocity Exoplanets with Astrometric Measurements". Research in Astronomy and Astrophysics. 23 (5): 055022. arXiv:2303.12409. Bibcode:2023RAA....23e5022X. doi:10.1088/1674-4527/accb7e. S2CID 257663647.