Observation data Epoch J2000.0 Equinox J2000.0 ( ICRS) | |
---|---|
Constellation | Telescopium |
Right ascension | 19h 27m 48.11739s [1] |
Declination | −54° 19′ 30.9786″ [1] |
Apparent magnitude (V) | 5.69±0.01 [2] |
Characteristics | |
Evolutionary stage | red giant branch [3] |
Spectral type | K4 III [4] |
U−B color index | +1.68 [5] |
B−V color index | +1.40 [5] |
Astrometry | |
Radial velocity (Rv) | −5±4.3 [6] km/s |
Proper motion (μ) |
RA: −5.554
mas/
yr
[1] Dec.: +9.807 mas/ yr [1] |
Parallax (π) | 5.1371 ± 0.0763 mas [1] |
Distance | 635 ± 9
ly (195 ± 3 pc) |
Absolute magnitude (MV) | −0.38 [7] |
Details | |
Mass | 1.12 [8] M☉ |
Radius | 32.6 [9] R☉ |
Luminosity | 329 [10] L☉ |
Surface gravity (log g) | 1.35 [8] cgs |
Temperature | 4,316±122 [9] K |
Metallicity [Fe/H] | −0.02 [8] dex |
Rotational velocity (v sin i) | <1 [11] km/s |
Other designations | |
Database references | |
SIMBAD | data |
HD 182509, also designated as HR 7370, is an orange hued star located in the southern constellation Telescopium. It has an apparent magnitude of 5.69, [2] making it faintly visible to the naked eye if viewed under ideal conditions. Parallax measurements place the object at a distance of 635 light years. [1] It has a poorly constrained heliocentric radial velocity of −5 km/s, [6] indicating that it is drifting towards the Solar System.
HD 182509 has a stellar classification of K4 III, [4] indicating that it is a red giant. Gaia DR3 stellar evolution models place it on the red giant branch. [3] It has 1.12 times the mass of the Sun [8] but has expanded to 32.6 times its girth. [9] It shines with a luminosity of 329 L☉ [10] from its enlarged photosphere at an effective temperature of 4,316 K. [9] HD 182509 iron abundance is 95% that of the Sun, placing it at solar metallicity. [8] Like most giants, it spins slowly with a projected rotational velocity of <1 km/s. [11]
HD 182466 is a high proper motion star located 76.1 ″ away along a position angle of 236°. [14] Eggleton and Tokovonin (2008) list the pair as a binary star. [15] However, its parallax and proper motion indicate that it is instead a foreground object. [16] Components C and D are instead faint optical background objects, while the E component is probably non-existent. [14]
Observation data Epoch J2000.0 Equinox J2000.0 ( ICRS) | |
---|---|
Constellation | Telescopium |
Right ascension | 19h 27m 48.11739s [1] |
Declination | −54° 19′ 30.9786″ [1] |
Apparent magnitude (V) | 5.69±0.01 [2] |
Characteristics | |
Evolutionary stage | red giant branch [3] |
Spectral type | K4 III [4] |
U−B color index | +1.68 [5] |
B−V color index | +1.40 [5] |
Astrometry | |
Radial velocity (Rv) | −5±4.3 [6] km/s |
Proper motion (μ) |
RA: −5.554
mas/
yr
[1] Dec.: +9.807 mas/ yr [1] |
Parallax (π) | 5.1371 ± 0.0763 mas [1] |
Distance | 635 ± 9
ly (195 ± 3 pc) |
Absolute magnitude (MV) | −0.38 [7] |
Details | |
Mass | 1.12 [8] M☉ |
Radius | 32.6 [9] R☉ |
Luminosity | 329 [10] L☉ |
Surface gravity (log g) | 1.35 [8] cgs |
Temperature | 4,316±122 [9] K |
Metallicity [Fe/H] | −0.02 [8] dex |
Rotational velocity (v sin i) | <1 [11] km/s |
Other designations | |
Database references | |
SIMBAD | data |
HD 182509, also designated as HR 7370, is an orange hued star located in the southern constellation Telescopium. It has an apparent magnitude of 5.69, [2] making it faintly visible to the naked eye if viewed under ideal conditions. Parallax measurements place the object at a distance of 635 light years. [1] It has a poorly constrained heliocentric radial velocity of −5 km/s, [6] indicating that it is drifting towards the Solar System.
HD 182509 has a stellar classification of K4 III, [4] indicating that it is a red giant. Gaia DR3 stellar evolution models place it on the red giant branch. [3] It has 1.12 times the mass of the Sun [8] but has expanded to 32.6 times its girth. [9] It shines with a luminosity of 329 L☉ [10] from its enlarged photosphere at an effective temperature of 4,316 K. [9] HD 182509 iron abundance is 95% that of the Sun, placing it at solar metallicity. [8] Like most giants, it spins slowly with a projected rotational velocity of <1 km/s. [11]
HD 182466 is a high proper motion star located 76.1 ″ away along a position angle of 236°. [14] Eggleton and Tokovonin (2008) list the pair as a binary star. [15] However, its parallax and proper motion indicate that it is instead a foreground object. [16] Components C and D are instead faint optical background objects, while the E component is probably non-existent. [14]