Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
---|---|
Constellation | Volans |
Right ascension | 08h 49m 50.12604s[1] |
Declination | −72° 33′ 04.4601″[1] |
Apparent magnitude (V) | 6.10±0.01[2] |
Characteristics | |
Spectral type | A5 III/IV[3] |
U−B color index | +0.17[4] |
B−V color index | +0.20[4] |
Astrometry | |
Radial velocity (Rv) | −2.6±1.1[5] km/s |
Proper motion (μ) | RA: −6.191 mas/yr[1] Dec.: +8.368 mas/yr[1] |
Parallax (π) | 1.3842 ± 0.0201 mas[1] |
Distance | 2,360 ± 30 ly (720 ± 10 pc) |
Details | |
Mass | 5.3[6] M☉ |
Radius | 22.9[7] R☉ |
Luminosity | 1,464±55[8] L☉ |
Surface gravity (log g) | 2.27[9] cgs |
Temperature | 8,121±123[7] K |
Metallicity [Fe/H] | −0.44[10] dex |
Other designations | |
Database references | |
SIMBAD | data |
HD 76270, also known as HR 3544, is a solitary, white hued star located in the southern circumpolar constellation Volans. It has an apparent magnitude of 6.10,[2] making it faintly visible to the naked eye if viewed under ideal conditions. The object is relatively far with a distance of 2,360 light years,[1] but is slowly approaching the Solar System with a heliocentric radial velocity of −2.6 km/s.[5]
HD 76270 was considered as a chemically peculiar Am star, and as a result, was given a spectral classification of A3mA6-7[3] by Nancy Houk and A.P Cowley. This means it is an A3 star with the metallic lines of a star with a class of A6-7. However, this peculiarity is now considered doubtful.[13] An alternate class of A5 III/IV[3] was given, instead making it an evolved A-type star with a blended luminosity class of a subgiant and a giant star.
At present it has 5.3 times the mass of the Sun[6] but has expanded to 22.9 times its girth.[7] It shines with a high luminosity of 1,464 L☉[8] from its enlarged photosphere at an effective temperature of 8,121 K.[7] HR 3544 is metal deficient, having an iron abundance 64% below solar levels.[10] A 1984 study used HD 76270 as a comparison star and suspected it of being slightly variable,[14] but this has not been confirmed and it is not even listed as a suspected variable in the General Catalogue of Variable Stars.[15]