Observation data Epoch J2000.0 Equinox J2000.0 ( ICRS) | |
---|---|
Constellation | Columba |
Right ascension | 05h 42m 15.19447s [2] |
Declination | −34° 40′ 04.1399″ [2] |
Apparent magnitude (V) | 5.28±0.01 [3] |
Characteristics | |
Evolutionary stage | main sequence [4] |
Spectral type | B9/9.5 V [5] |
B−V color index | −0.05 [6] |
Variable type | SPB [7] or α2 CVn [8] |
Astrometry | |
Radial velocity (Rv) | 36.3±0.6 [9] km/s |
Proper motion (μ) |
RA: +5.081
mas/
yr
[2] Dec.: +51.365 mas/ yr [2] |
Parallax (π) | 8.929 ± 0.08896 mas [2] |
Distance | 365 ± 4
ly (112 ± 1 pc) |
Absolute magnitude (MV) | −0.3 [10] |
Details | |
Mass | 3.07±0.05 [4] M☉ |
Radius | 3.47 [11] R☉ |
Luminosity | 124 [12] L☉ |
Surface gravity (log g) | 3.79±0.07 [13] cgs |
Temperature | 10,000+256 −250 [4] K |
Metallicity [Fe/H] | +0.51 [14] dex |
Rotational velocity (v sin i) | 65±5 [15] km/s |
Age | 394+10 −17 [16] Myr |
Other designations | |
Database references | |
SIMBAD | data |
WZ Columbae, also known as HD 38170, is a solitary, [19] bluish-white hued star located in the southern constellation Columba, the dove. It has an apparent magnitude of 5.28, [3] allowing it to be faintly visible to the naked eye. Based on parallax measurements from the Gaia spacecraft, the object is about 365 light years distant. [2] It appears to be receding from the Solar System, having a heliocentric radial velocity of 36.3 km/s. [9]
WZ Columbae was originally listed as a slowly pulsating B-type star by the General Catalogue of Variable Stars. However, observations from Hempel & Howlger (2003) reveal it to be overabundant in strontium and barium. [14] Combined with Hipparcos photometry, this led to the object being reclassified as an Alpha2 Canum Venaticorum variable. [8] Based on data collected in the Hipparcos passband, it fluctuates between magnitudes 5.27 and 5.29 over 1.38 days. [7] [20] However, TESS data suggests a period of 2.76618±0.00004 days; double that of the earlier data. [16]
The stellar classification of WZ Columbae is B9/9.5 V [5] — a main-sequence star with the characteristics of a B9 and B9.5 star. It has 3.07 [4] times the mass of the Sun and is estimated to be 394 million years old, [16] having completed 89.2% of its main sequence lifetime. [4] It has a slightly enlarged radius of 3.47 R☉ [11] and an effective temperature of 10,000 K. [4] This yields a luminosity 124 times that of the Sun [12] from its photosphere. Like most chemically peculiar stars, WZ Columbae has a relatively slow projected rotational velocity at 65 km/s. [15]
Observation data Epoch J2000.0 Equinox J2000.0 ( ICRS) | |
---|---|
Constellation | Columba |
Right ascension | 05h 42m 15.19447s [2] |
Declination | −34° 40′ 04.1399″ [2] |
Apparent magnitude (V) | 5.28±0.01 [3] |
Characteristics | |
Evolutionary stage | main sequence [4] |
Spectral type | B9/9.5 V [5] |
B−V color index | −0.05 [6] |
Variable type | SPB [7] or α2 CVn [8] |
Astrometry | |
Radial velocity (Rv) | 36.3±0.6 [9] km/s |
Proper motion (μ) |
RA: +5.081
mas/
yr
[2] Dec.: +51.365 mas/ yr [2] |
Parallax (π) | 8.929 ± 0.08896 mas [2] |
Distance | 365 ± 4
ly (112 ± 1 pc) |
Absolute magnitude (MV) | −0.3 [10] |
Details | |
Mass | 3.07±0.05 [4] M☉ |
Radius | 3.47 [11] R☉ |
Luminosity | 124 [12] L☉ |
Surface gravity (log g) | 3.79±0.07 [13] cgs |
Temperature | 10,000+256 −250 [4] K |
Metallicity [Fe/H] | +0.51 [14] dex |
Rotational velocity (v sin i) | 65±5 [15] km/s |
Age | 394+10 −17 [16] Myr |
Other designations | |
Database references | |
SIMBAD | data |
WZ Columbae, also known as HD 38170, is a solitary, [19] bluish-white hued star located in the southern constellation Columba, the dove. It has an apparent magnitude of 5.28, [3] allowing it to be faintly visible to the naked eye. Based on parallax measurements from the Gaia spacecraft, the object is about 365 light years distant. [2] It appears to be receding from the Solar System, having a heliocentric radial velocity of 36.3 km/s. [9]
WZ Columbae was originally listed as a slowly pulsating B-type star by the General Catalogue of Variable Stars. However, observations from Hempel & Howlger (2003) reveal it to be overabundant in strontium and barium. [14] Combined with Hipparcos photometry, this led to the object being reclassified as an Alpha2 Canum Venaticorum variable. [8] Based on data collected in the Hipparcos passband, it fluctuates between magnitudes 5.27 and 5.29 over 1.38 days. [7] [20] However, TESS data suggests a period of 2.76618±0.00004 days; double that of the earlier data. [16]
The stellar classification of WZ Columbae is B9/9.5 V [5] — a main-sequence star with the characteristics of a B9 and B9.5 star. It has 3.07 [4] times the mass of the Sun and is estimated to be 394 million years old, [16] having completed 89.2% of its main sequence lifetime. [4] It has a slightly enlarged radius of 3.47 R☉ [11] and an effective temperature of 10,000 K. [4] This yields a luminosity 124 times that of the Sun [12] from its photosphere. Like most chemically peculiar stars, WZ Columbae has a relatively slow projected rotational velocity at 65 km/s. [15]