| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Andromeda |
| Right ascension | 00h 13m 23.9130s[1] |
| Declination | +26° 59′ 14.9814″[1] |
| Apparent magnitude (V) | 6.277[2] |
| Characteristics | |
| Spectral type | G0III+F2IV[3] |
| B−Vcolor index | 0.63[2] |
| Astrometry | |
| Radial velocity (Rv) | −5.99±0.18[1] km/s |
| Proper motion (μ) | RA: −11.915±1.179[1]mas/yr Dec.: −22.820±1.161[1]mas/yr |
| Parallax (π) | 18.6899±0.7533 mas[1] |
| Distance | 175 ± 7 ly (54 ± 2 pc) |
| Orbit[3] | |
| Primary | HD 895A |
| Companion | HD 895B |
| Period (P) | 421yr |
| Semi-major axis (a) | 0.641″ |
| Eccentricity (e) | 0.720 |
| Inclination (i) | 124.10° |
| Longitude of the node (Ω) | 193° |
| Periastronepoch (T) | JD 2,401,969.97 |
| Argument of periastron (ω) (secondary) | 286.1° |
| Details[3] | |
| HD 895A | |
| Mass | 2.42 M☉ |
| HD 895B | |
| Mass | 1.92 M☉ |
| Other designations | |
| SAO 73823,WDS J00134+2659,HD 895,BD+26° 13,HIP 1076,HR 40. | |
| Database references | |
| SIMBAD | data |
| Database references | |
| SIMBAD | data |
HD 895 is amultiple star system in the constellationAndromeda. Its apparent magnitude is 6.277,[2] so it can be seen by the naked eye under very favourable conditions. Based on parallax measured byHipparcos, the system is located around 54 parsecs (180 ly) away,[4] and it is made of two differentspectroscopic binary pairs.[5]
The first pair is made of a primaryyellow giant star ofspectral type G0III, and the secondarysubgiant star of spectral type K2IV, so they have both left themain sequence evolutionary phase. They are also both more massive than theSun. The secondary completes an orbit around the primary every 421years.[3]
The second pair is a double-lined spectroscopic binary located 18arcseconds away from the first pair, although with an apparent magnitude of 10.37 it is too faint to be seen without a telescope. It was not recognized as a separate pair in the oldBright Star Catalogue andHenry Draper Catalogue, thus it bears the designationHD 895C. They are bothG-type main sequence stars slightly less massive than the Sun, with spectral types G7V and G8V respectively. They complete an orbit around theircenter of mass approximately every 6 days.[3]
UsingGaia parallax, instead, the pair formed by the primary and the secondary is much closer than previous measures, at an estimated distance of 175light years. The two pairs, then, may be not gravitationally bound.[1]
| Stars |
| ||||||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| |||||||||||||
| Star clusters |
| ||||||||||||
| Nebulae |
| ||||||||||||
| Galaxies |
| ||||||||||||
| |||||||||||||
| |||||||||||||
 | This binary or multiple star system–related article is astub. You can help Wikipedia byexpanding it. |
