HR 1614
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| Observation data Epoch J2000 |
|
|---|---|
| Constellation (pronunciation) |
Eridanus |
| Right ascension | 05h 00m 49.0001s |
| Declination | -05° 45′ 13.231″ |
| Apparent magnitude (V) | 6.22 |
| Characteristics | |
| Spectral type | K3 V |
| U-B color index | 1.02 |
| B-V color index | 1.06 |
| Variable type | None |
| Astrometry | |
| Radial velocity (Rv) | +27 km/s |
| Proper motion (μ) | RA: 550.71 mas/yr Dec.: -1109.24 mas/yr |
| Parallax (π) | 113.46 ± 0.82 mas |
| Distance | 28.7 ± 0.2 ly (8.81 ± 0.06 pc) |
| Absolute magnitude (MV) | 6.49 |
| Details | |
| Mass | 0.845 M☉ |
| Radius | 0.81 R☉ |
| Luminosity | 0.21 L☉ |
| Temperature | 4614 K |
| Metallicity | 190% Sun |
| Rotation | ? |
| Age | 2 × 109 years |
| Other designations | |
HR 1614 is a spectroscopic binary star system in the constellation Eridanus. (The information in the table is for the primary star.)
It is considered a metal-rich dwarf star, which means it displays an unusually high portion of elements heavier than Helium in its spectrum. This metallicity is given in term of the ratio of Iron to Hydrogen, as compared to the Sun. In the case of HR 1614, this ratio is about 90% higher than the Sun.[2] The activity cycle for this star is 11.1 years in length.[3]
This system is a member of a moving group of at least nine stars that share a common motion through space. The members of this group display the same abundance of heavy elements as does HR 1614, which may indicate a common origin for these stars. The space velocity of this group relative to the Sun is 59 km/s.[4] The estimated age of this group is 2 Gyr.[5]
[edit] References
- ^ HD 32147 -- High proper-motion Star (English). Centre de Données astronomiques de Strasbourg. Retrieved on 2006-06-08.
- ^ S. Feltzing, G. Gonzalez (2001). "The nature of super-metal-rich stars. Detailed abundance analysis of 8 super-metal-rich star candidates". Astronomy and Astrophysics 367 (2): 253–265. doi:.
- ^ H-K Project: Activity Cycles. Mt. Wilson Observatory. Retrieved on 2006-11-30.
- ^ Eggen, O. J. (1992). "HR 1614 and the dissolution of a supercluster". Astronomical Journal 104 (5): 1906–1915. doi:.
- ^ S. Feltzing, J. Holmberg (2000). "The reality of old moving groups - the case of HR 1614. Age, metallicity, and a new extended sample". Astronomy and Astrophysics 357: 153–163.
