Observation data Epoch J2000.0 Equinox J2000.0 ( ICRS) | |
---|---|
Constellation | Hercules |
Right ascension | 16h 08m 46.17745s [1] |
Declination | +44° 56′ 05.6663″ [1] |
Apparent magnitude (V) | 4.24 [2] |
Characteristics | |
Spectral type | B9VspHgMn [3] + A8V [4] |
U−B color index | −0.23 [2] |
B−V color index | −0.06 [2] |
Variable type | α2 CVn? [5] |
Astrometry | |
Radial velocity (Rv) | −16.3±0.4 [6] km/s |
Proper motion (μ) |
RA: −26.63
[1]
mas/
yr Dec.: +36.76 [1] mas/ yr |
Parallax (π) | 15.99 ± 0.45 mas [1] |
Distance | 204 ± 6
ly (63 ± 2 pc) |
Absolute magnitude (MV) | A: 0.100 ± 0.059 B: 2.670 ± 0.074 [7] |
Orbit [7] | |
Period (P) | 564.834±0.038 d |
Semi-major axis (a) | 32.027±0.028 mas |
Eccentricity (e) | 0.52614±0.00086 |
Inclination (i) | 9.1±0.4° |
Longitude of the node (Ω) | 190.4±1.4° |
Periastron epoch (T) | 2450121.43 ± 0.20 JD |
Argument of periastron (ω) (secondary) | 350.3±1.4° |
Semi-amplitude (K1) (primary) | 2.772±0.073 km/s |
Semi-amplitude (K2) (secondary) | 8.1 [4] km/s |
Details | |
φ Her A | |
Mass | 3.05±0.24 [7] M☉ |
Luminosity | 72 [8] L☉ |
Surface gravity (log g) | 4.05±0.15 [4] cgs |
Temperature | 11,525±150 [4] K |
Metallicity [Fe/H] | −0.03 [7] dex |
Rotational velocity (v sin i) | 8.0±1.0 [4] km/s |
Age | 210 [7] Myr |
φ Her B | |
Mass | 1.614±0.066 [7] M☉ |
Surface gravity (log g) | 4.30±0.15 [4] cgs |
Temperature | 8,000±150 [4] K |
Rotational velocity (v sin i) | 50.0±3.0 [4] km/s |
Other designations | |
Database references | |
SIMBAD | data |
Phi Herculis (φ Her) is a binary star [4] system in the northern constellation of Hercules. Based upon an annual parallax shift of 15.99 mas as seen from Earth, [1] it is located around 204 light years from the Sun. With a combined apparent visual magnitude of 4.24, [2] it is bright enough to be seen with the naked eye.
This is a single-lined spectroscopic binary star system with an orbital period of 564.8 days and an eccentricity of 0.526. [7] The primary, component A, is a B-type main sequence star with a stellar classification of B9VspHgMn. [3] It is a chemically peculiar star of the type called a mercury-manganese star. [4] The star is tentatively catalogued as an Alpha2 Canum Venaticorum variable, with brightness variations of just 0.01 magnitudes. [5] [12]
The secondary, component B, was first separated via interferometry in 2004. [13] It is an A-type main sequence star of class A8V. [4] The magnitude difference between the two components is 2.64. [13]
Observation data Epoch J2000.0 Equinox J2000.0 ( ICRS) | |
---|---|
Constellation | Hercules |
Right ascension | 16h 08m 46.17745s [1] |
Declination | +44° 56′ 05.6663″ [1] |
Apparent magnitude (V) | 4.24 [2] |
Characteristics | |
Spectral type | B9VspHgMn [3] + A8V [4] |
U−B color index | −0.23 [2] |
B−V color index | −0.06 [2] |
Variable type | α2 CVn? [5] |
Astrometry | |
Radial velocity (Rv) | −16.3±0.4 [6] km/s |
Proper motion (μ) |
RA: −26.63
[1]
mas/
yr Dec.: +36.76 [1] mas/ yr |
Parallax (π) | 15.99 ± 0.45 mas [1] |
Distance | 204 ± 6
ly (63 ± 2 pc) |
Absolute magnitude (MV) | A: 0.100 ± 0.059 B: 2.670 ± 0.074 [7] |
Orbit [7] | |
Period (P) | 564.834±0.038 d |
Semi-major axis (a) | 32.027±0.028 mas |
Eccentricity (e) | 0.52614±0.00086 |
Inclination (i) | 9.1±0.4° |
Longitude of the node (Ω) | 190.4±1.4° |
Periastron epoch (T) | 2450121.43 ± 0.20 JD |
Argument of periastron (ω) (secondary) | 350.3±1.4° |
Semi-amplitude (K1) (primary) | 2.772±0.073 km/s |
Semi-amplitude (K2) (secondary) | 8.1 [4] km/s |
Details | |
φ Her A | |
Mass | 3.05±0.24 [7] M☉ |
Luminosity | 72 [8] L☉ |
Surface gravity (log g) | 4.05±0.15 [4] cgs |
Temperature | 11,525±150 [4] K |
Metallicity [Fe/H] | −0.03 [7] dex |
Rotational velocity (v sin i) | 8.0±1.0 [4] km/s |
Age | 210 [7] Myr |
φ Her B | |
Mass | 1.614±0.066 [7] M☉ |
Surface gravity (log g) | 4.30±0.15 [4] cgs |
Temperature | 8,000±150 [4] K |
Rotational velocity (v sin i) | 50.0±3.0 [4] km/s |
Other designations | |
Database references | |
SIMBAD | data |
Phi Herculis (φ Her) is a binary star [4] system in the northern constellation of Hercules. Based upon an annual parallax shift of 15.99 mas as seen from Earth, [1] it is located around 204 light years from the Sun. With a combined apparent visual magnitude of 4.24, [2] it is bright enough to be seen with the naked eye.
This is a single-lined spectroscopic binary star system with an orbital period of 564.8 days and an eccentricity of 0.526. [7] The primary, component A, is a B-type main sequence star with a stellar classification of B9VspHgMn. [3] It is a chemically peculiar star of the type called a mercury-manganese star. [4] The star is tentatively catalogued as an Alpha2 Canum Venaticorum variable, with brightness variations of just 0.01 magnitudes. [5] [12]
The secondary, component B, was first separated via interferometry in 2004. [13] It is an A-type main sequence star of class A8V. [4] The magnitude difference between the two components is 2.64. [13]