Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Cepheus |
Right ascension | 20h 45m 21.12879s [1] |
Declination | +57° 34′ 47.0080″ [1] |
Apparent magnitude (V) | 4.51 [2] |
Characteristics | |
Spectral type | F8IV-V + F9IV-V [2] |
Astrometry | |
Radial velocity (Rv) | −32.82±0.04 [3] km/s |
Proper motion (μ) |
RA: −62.32
[1]
mas/
yr Dec.: −236.00 [1] mas/ yr |
Parallax (π) | 36.64 ± 0.48 mas [1] |
Distance | 89 ± 1
ly (27.3 ± 0.4 pc) |
Absolute magnitude (MV) | 2.35 [4] |
Orbit [2] | |
Period (P) | 494.16±0.58 d |
Semi-major axis (a) | 0.065±0.001" (≥50.2±0.5 Gm [5]) |
Eccentricity (e) | 0.551±0.004 |
Inclination (i) | 24.53±3.13° |
Longitude of the node (Ω) | 325.21±1.05° |
Periastron epoch (T) | B 1996.335 ± 0.0017 |
Argument of periastron (ω) (secondary) | 68.86±0.76° |
Details [2] | |
HR 7955 A | |
Mass | 1.071±0.037 M☉ |
Age | 2.25 [6] Gyr |
HR 7955 B | |
Mass | 1.047±0.037 M☉ |
Other designations | |
Database references | |
SIMBAD | data |
HR 7955 is a binary star [2] system in the northern circumpolar constellation of Cepheus, near the constellation border with Cygnus. It has a yellow-white hue and is faintly visible to the naked eye with a combined apparent visual magnitude of 4.51. [2] The system is located at a distance of 89 light-years (27.3 parsecs) from the Sun, based on parallax. [1] It has a relatively high proper motion, traversing the celestial sphere at the rate of 0.243 arc seconds per annum, [8] and is drifting closer to the Sun with a radial velocity of -33 km/s. [3]
The double-lined nature of this spectroscopic binary system was not announced until 1972. [5] It has an orbital period of 1.35 years and an eccentricity of 0.551. [2] Both components appear to be slightly evolved stars that are leaving the main sequence and becoming subgiant stars, with stellar classifications of F8IV-V and F9IV-V. They each have slightly greater mass than the Sun: 107% and 105%, respectively. [2] The system is about 2.25 billion years old. [6]
Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Cepheus |
Right ascension | 20h 45m 21.12879s [1] |
Declination | +57° 34′ 47.0080″ [1] |
Apparent magnitude (V) | 4.51 [2] |
Characteristics | |
Spectral type | F8IV-V + F9IV-V [2] |
Astrometry | |
Radial velocity (Rv) | −32.82±0.04 [3] km/s |
Proper motion (μ) |
RA: −62.32
[1]
mas/
yr Dec.: −236.00 [1] mas/ yr |
Parallax (π) | 36.64 ± 0.48 mas [1] |
Distance | 89 ± 1
ly (27.3 ± 0.4 pc) |
Absolute magnitude (MV) | 2.35 [4] |
Orbit [2] | |
Period (P) | 494.16±0.58 d |
Semi-major axis (a) | 0.065±0.001" (≥50.2±0.5 Gm [5]) |
Eccentricity (e) | 0.551±0.004 |
Inclination (i) | 24.53±3.13° |
Longitude of the node (Ω) | 325.21±1.05° |
Periastron epoch (T) | B 1996.335 ± 0.0017 |
Argument of periastron (ω) (secondary) | 68.86±0.76° |
Details [2] | |
HR 7955 A | |
Mass | 1.071±0.037 M☉ |
Age | 2.25 [6] Gyr |
HR 7955 B | |
Mass | 1.047±0.037 M☉ |
Other designations | |
Database references | |
SIMBAD | data |
HR 7955 is a binary star [2] system in the northern circumpolar constellation of Cepheus, near the constellation border with Cygnus. It has a yellow-white hue and is faintly visible to the naked eye with a combined apparent visual magnitude of 4.51. [2] The system is located at a distance of 89 light-years (27.3 parsecs) from the Sun, based on parallax. [1] It has a relatively high proper motion, traversing the celestial sphere at the rate of 0.243 arc seconds per annum, [8] and is drifting closer to the Sun with a radial velocity of -33 km/s. [3]
The double-lined nature of this spectroscopic binary system was not announced until 1972. [5] It has an orbital period of 1.35 years and an eccentricity of 0.551. [2] Both components appear to be slightly evolved stars that are leaving the main sequence and becoming subgiant stars, with stellar classifications of F8IV-V and F9IV-V. They each have slightly greater mass than the Sun: 107% and 105%, respectively. [2] The system is about 2.25 billion years old. [6]