HD 50554

Last updated
HD 50554
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Gemini [1]
Right ascension 06h 54m 42.82615s [2]
Declination +24° 14′ 44.0057″ [2]
Apparent magnitude  (V)+6.84 [1]
Characteristics
Evolutionary stage main sequence [2]
Spectral type F8V [3]
B−V color index 0.582±0.008 [1]
Astrometry
Radial velocity (Rv)−3.77±0.13 [2] km/s
Proper motion (μ)RA: −35.839 mas/yr [2]
Dec.: −96.668 mas/yr [2]
Parallax (π)32.1855±0.0242  mas [2]
Distance 101.34 ± 0.08  ly
(31.07 ± 0.02  pc)
Absolute magnitude  (MV)4.46 [1]
Details
Mass 1.06±0.03 [4]   M☉
Radius 1.07±0.03 [4]   R☉
Luminosity 1.37±0.01 [4]   L☉
Surface gravity (log g)4.4±0.04 [4]   cgs
Temperature 6,036±52 [4]   K
Metallicity [Fe/H]0.05±0.06 [5]   dex
Rotational velocity (v sin i)2.3 [5]  km/s
Age 3.3±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
SIMBAD data

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, [1] 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. [2]

Contents

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 ° —
Disk45 AU ——

See also

References

  1. 1 2 3 4 5 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. XHIP record for this object at VizieR.
  2. 1 2 3 4 5 6 7 8 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.
  3. 1 2 3 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. 1 2 3 4 5 6 7 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. 1 2 3 4 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. 1 2 3 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. 1 2 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. 1 2 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.
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.