HD 110073
Star in the constellation Centaurus
From Wikipedia, the free encyclopedia
HD 110073 is a star in the southern constellation Centaurus, near the southern constellation border with Crux. It has the Bayer designation l Centauri (lower case L), while HD 110073 is the star's identifier from the Henry Draper catalogue. This system is faintlyvisible to the naked eye with an apparent visual magnitude of +4.63.[1] It is located at a distance of approximately 365 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +15 km/s.[1]
 | |
| Observation data Epoch J2000.0 Equinox ICRS | |
|---|---|
| Constellation | Centaurus[1] |
| Right ascension | 12h 39m 52.52839s[2] |
| Declination | −55° 58′ 31.8904″[2] |
| Apparent magnitude (V) | +4.63[1] |
| Characteristics | |
| Spectral type | B8II/III[3] |
| B−V color index | −0.082±0.013[1] |
| Astrometry | |
| Radial velocity (Rv) | +15.1±2.8[1] km/s |
| Proper motion (μ) | RA: −43.38[2] mas/yr Dec.: −25.25[2] mas/yr |
| Parallax (π) | 8.94±0.24 mas[2] |
| Distance | 365 ± 10 ly (112 ± 3 pc) |
| Absolute magnitude (MV) | −0.61[1] |
| Details | |
| HD 110073 A | |
| Mass | 4.0±0.2[4] M☉ |
| Radius | 3.7[5] R☉ |
| Luminosity | 385[4] L☉ |
| Surface gravity (log g) | 3.35[6] cgs |
| Temperature | 12,900[4] K |
| Metallicity [Fe/H] | −0.90[6] dex |
| Rotation | 3.03 days[7] |
| Rotational velocity (v sin i) | 46±10[8] km/s |
| Age | 129[4] Myr |
| HD 110073 B | |
| Mass | 1.13[4] M☉ |
| Luminosity | 1.2[4] L☉ |
| Temperature | 5,662[4] K |
| Other designations | |
| l Cen, CD−39°7748, HD 110073, HIP 61789, HR 4817, SAO 203681[9] | |
| Database references | |
| SIMBAD | data |
This is a single-lined spectroscopic binary star system that belongs to the Pleiades stream.[4] As of 2011, the pair had a linear projected separation of 130.8±12.1 AU.[10] The primary component is a mercury-manganese star[6] with a stellar classification of B8II/III.[3] These stars are often helium-weak, but this is one of the most normal members of this group in terms of helium abundance.[11] The system is a source for X-ray emission, which is most likely coming from the lower mass companion – it may even be a pre-main-sequence star.[4]