Observation data Epoch J2000.0 Equinox J2000.0 ( ICRS) | |
---|---|
Constellation | Apus |
Right ascension | 17h 12m 19.93421s [1] |
Declination | −70° 43′ 15.8963″ [1] |
Apparent magnitude (V) | 6.21±0.01 [2] |
Characteristics | |
Evolutionary stage | subgiant |
Spectral type | K1 IV CN3 [3] |
U−B color index | +1.04 [4] |
B−V color index | +1.06 [4] |
Astrometry | |
Radial velocity (Rv) | −24±0.4 [5] km/s |
Proper motion (μ) |
RA: +49.060
mas/
yr
[1] Dec.: −78.104 mas/ yr [1] |
Parallax (π) | 14.3386 ± 0.0224 mas [1] |
Distance | 227.5 ± 0.4
ly (69.7 ± 0.1 pc) |
Absolute magnitude (MV) | +2.10 [6] |
Details | |
Mass | 1.25 [7] M☉ |
Radius | 6.35±0.32 [8] R☉ |
Luminosity | 19.7±0.1 [1] L☉ |
Surface gravity (log g) | 2.90±0.25 [9] cgs |
Temperature | 4,677 [10] K |
Metallicity [Fe/H] | +0.04±0.09 [9] dex |
Rotational velocity (v sin i) | <1 [11] km/s |
Age | 3.52+0.36 −0.37 [1] Gyr |
Other designations | |
Database references | |
SIMBAD | data |
HD 154556, also known as HR 6357, is a solitary orange-hued star located in the southern circumpolar constellation Apus. It has an apparent magnitude of 6.21, [2] placing it near the limit for naked eye visibility. The star is located relatively close at a distance of 228 light years based on Gaia DR3 parallax measurements, [1] but it is drifter closer with a heliocentric radial velocity of −24 km/s. [5] At its current distance, HD 154556's brightness is diminished by 0.26 magnitudes due to interstellar dust. [14] It has an absolute magnitude of +2.10. [6]
HD 154556 has a stellar classification of K1 IV CN3, [3] indicating that it is an evolved K-type subgiant with a moderate abundance of cyano radicals in its spectrum, making it a CN star. It has 1.25 times the mass of the Sun [7] and is calculated to be 3.52 billion years old, [1] having expanded to 6.35 times the radius of the Sun. [8] It now radiates 19.7 times the luminosity of the Sun [1] from its enlarged photosphere at an effective temperature of 4,677 K. [10] It has a near solar metallicity [9] and spins slowly with a projected rotational velocity lower than 1 km/s. [11]
Observation data Epoch J2000.0 Equinox J2000.0 ( ICRS) | |
---|---|
Constellation | Apus |
Right ascension | 17h 12m 19.93421s [1] |
Declination | −70° 43′ 15.8963″ [1] |
Apparent magnitude (V) | 6.21±0.01 [2] |
Characteristics | |
Evolutionary stage | subgiant |
Spectral type | K1 IV CN3 [3] |
U−B color index | +1.04 [4] |
B−V color index | +1.06 [4] |
Astrometry | |
Radial velocity (Rv) | −24±0.4 [5] km/s |
Proper motion (μ) |
RA: +49.060
mas/
yr
[1] Dec.: −78.104 mas/ yr [1] |
Parallax (π) | 14.3386 ± 0.0224 mas [1] |
Distance | 227.5 ± 0.4
ly (69.7 ± 0.1 pc) |
Absolute magnitude (MV) | +2.10 [6] |
Details | |
Mass | 1.25 [7] M☉ |
Radius | 6.35±0.32 [8] R☉ |
Luminosity | 19.7±0.1 [1] L☉ |
Surface gravity (log g) | 2.90±0.25 [9] cgs |
Temperature | 4,677 [10] K |
Metallicity [Fe/H] | +0.04±0.09 [9] dex |
Rotational velocity (v sin i) | <1 [11] km/s |
Age | 3.52+0.36 −0.37 [1] Gyr |
Other designations | |
Database references | |
SIMBAD | data |
HD 154556, also known as HR 6357, is a solitary orange-hued star located in the southern circumpolar constellation Apus. It has an apparent magnitude of 6.21, [2] placing it near the limit for naked eye visibility. The star is located relatively close at a distance of 228 light years based on Gaia DR3 parallax measurements, [1] but it is drifter closer with a heliocentric radial velocity of −24 km/s. [5] At its current distance, HD 154556's brightness is diminished by 0.26 magnitudes due to interstellar dust. [14] It has an absolute magnitude of +2.10. [6]
HD 154556 has a stellar classification of K1 IV CN3, [3] indicating that it is an evolved K-type subgiant with a moderate abundance of cyano radicals in its spectrum, making it a CN star. It has 1.25 times the mass of the Sun [7] and is calculated to be 3.52 billion years old, [1] having expanded to 6.35 times the radius of the Sun. [8] It now radiates 19.7 times the luminosity of the Sun [1] from its enlarged photosphere at an effective temperature of 4,677 K. [10] It has a near solar metallicity [9] and spins slowly with a projected rotational velocity lower than 1 km/s. [11]