HD 50554
| Observation data Epoch J2000.0 Equinox ICRS | |
|---|---|
| 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 |
| Exoplanet Archive | 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]
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
[edit]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] Two more inner planet candidates, both super-Earths, have been detected by TESS; they were validated by a 2026 study.[12]
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]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination (°) |
Radius |
|---|---|---|---|---|---|---|
| c[12] | <5.3 M🜨 | 0.066+0.009 −0.018 |
5.969362(20) | — | — | 1.31±0.06 R🜨 |
| d[12] | <10.4 M🜨 | 0.168+0.028 −0.065 |
28.06940(40) | — | — | 1.41+0.14 −0.09 R🜨 |
| b[13] | 4.88+0.31 −0.26 MJ |
2.274±0.029 | 1,223.1+2.0 −1.9 |
0.456+0.019 −0.018 |
111.0±6.5 | — |
| Disk[8] | 45 AU | — | — | |||
See also
[edit]References
[edit]- 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.
- 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.
- 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.
- 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.
- 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.
- ↑ "HD 50554". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2021-10-24.
- ↑ 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.
- 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.
- 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.
- ↑ "Exoplanets: The Hunt Continues!" (Press release). Garching, Germany: European Southern Observatory. April 4, 2001. Retrieved December 27, 2012.
- ↑ 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.
- 1 2 3 Liu, Quanyi; Zhu, Wei; Gan, Tianjun; Dai, Fei (February 2026). "TESS planets in known radial velocity cold Jupiter systems: Hot super Earth occurrence is enhanced by cold Jupiters". The Astronomical Journal. arXiv:2602.11017.
- ↑ Xiao, Guang-Yao; Teng, Huan-Yu; et al. (September 2026). "Transiting Planetary Systems with Distant Giant Companions Remain Moderately Coplanar". The Astrophysical Journal Letters. arXiv:2609.01377.
