HD 90132
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  | |
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Antlia[1] |
| Right ascension | 10h 23m 29.29608s[2] |
| Declination | −38° 00′ 35.4255″[2] |
| Apparent magnitude (V) | 5.33±0.01[3] |
| Characteristics | |
| Spectral type | A8 V[4] |
| B−V color index | +0.25[5] |
| Astrometry | |
| Radial velocity (Rv) | 17±4.2[6] km/s |
| Proper motion (μ) | RA: −158.833 mas/yr[2] Dec.: −53.705 mas/yr[2] |
| Parallax (π) | 24.2034±0.0725 mas[2] |
| Distance | 134.8 ± 0.4 ly (41.3 ± 0.1 pc) |
| Absolute magnitude (MV) | +2.25[1] |
| Details | |
| Mass | 1.69±0.27[7] M☉ |
| Radius | 1.87±0.87[7] R☉ |
| Luminosity | 9.79±0.06[8] L☉ |
| Surface gravity (log g) | 4.15[9] cgs |
| Temperature | 7,737±263[9] K |
| Metallicity [Fe/H] | −0.13[10] dex |
| Rotational velocity (v sin i) | 270[11] km/s |
| Age | 70[12] Myr |
| Other designations | |
| 64 G. Antliae[13], CD−37°6509, CPD−37°4123, FK5 1269, GC 14281, HD 90132, HIP 50888, HR 4086, SAO 201346[14] | |
| Database references | |
| SIMBAD | data |
HD 90132 (HR 4086) is a solitary[15] white hued star located in the southern constellation Antlia. It has an apparent magnitude of 5.33,[3] making it one of the brighter members of this generally faint constellation. The star is relatively close at a distance of 135 light years[2] but is receding with a heliocentric radial velocity of 17 km/s.[6]
HD 90132 has a stellar classification of A8 V,[4] indicating that it is an ordinary A-type main-sequence star. At present it has 1.69 times the mass of the Sun and 1.87 times the radius of the Sun.[7] Despite a young age of 70 million years,[12] the star has a lower surface gravity than expected.[9] This is due to the equator being 18% larger than the poles,[16] which is due to a high projected rotational velocity of 270 km/s.[11] Nevertheless, it shines with a luminosity of 9.8 L☉[8] from its photosphere at an effective temperature of 7,737 K.[9] HD 90132 is slightly metal deficient with a metallicity 74% that of Sun.[10]
This star was observed for infrared excess suggesting the presence of a circumstellar disk, but as of 2017 no excess have been found.[17]
