  | |
| Observation data Epoch J2000 Equinox ICRS | |
|---|---|
| Constellation | Lynx |
| Right ascension | 06h 19m 37.38458s |
| Declination | +59° 00′ 39.4683″ |
| Apparent magnitude (V) | 4.44 |
| Characteristics | |
| Evolutionary stage | main sequence |
| Spectral type | A2 Vs |
| B−V color index | 0.032±0.004 |
| Variable type | Eclipsing binary |
| Astrometry | |
| Radial velocity (Rv) | −2.0±0.1 km/s |
| Proper motion (μ) | RA: −5.35 mas/yr Dec.: +23.86 mas/yr |
| Parallax (π) | 20.83±0.40 mas |
| Distance | 157 ± 3 ly (48.0 ± 0.9 pc) |
| Absolute magnitude (MV) | 1.03 |
| Orbit | |
| Period (P) | 1306.82±0.96 d |
| Eccentricity (e) | 0.497±0.010 |
| Periastron epoch (T) | 2450962.0±2.0 |
| Argument of periastron (ω) (secondary) | 186.30±0.79° |
| Semi-amplitude (K1) (primary) | 3.281±0.044 km/s |
| Details | |
| 2 Lyn A | |
| Mass | 2.32±0.02 M☉ |
| Radius | 2.2 R☉ |
| Luminosity | 39.5+1.8 −1.7 L☉ |
| Surface gravity (log g) | 4.1±0.1 cgs |
| Temperature | 9,310±100 K |
| Rotation | 1.56 d |
| Rotational velocity (v sin i) | 44 km/s |
| 2 Lyn B | |
| Mass | 0.46 M☉ |
| Other designations | |
| 2 Lyn, UZ Lyn, BD+59°959, FK5 237, HD 43378, HIP 30060, HR 2238, SAO 25665 | |
| Database references | |
| SIMBAD | data |
2 Lyncis is a binary star system in the northern constellation Lynx. It is visible to the naked eye, having an apparent visual magnitude of 4.44. The distance to this system, judging by an annual parallax shift of 20.83±0.40 mas, is around 157 light years. It is moving closer to the Sun with a heliocentric radial velocity of −2 km/s.
This is a spectroscopic binary star system with an orbital period of around 3.6 years and an eccentricity of 0.5. It is classified as a probable (91% chance) eclipsing binary with the variable star designation UZ Lyn, showing a net magnitude decrease of 0.3 during an occultation.
The primary component is an A-type main-sequence star with a stellar classification of A2 Vs, where the 's' indicates narrow (sharp) absorption lines. The orbiting companion may be the source of the X-ray emission from this system, as stars similar to the primary component do not generally produce detectable levels of X-rays.
