QZ Puppis

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QZ Puppis
Puppis constellation map.svg
Red circle.svg
Location of QZ Puppis (circled)
Observation data
Epoch J2000       Equinox J2000
Constellation Puppis
Right ascension 07h 52m 38.64663s [1]
Declination −38° 51 46.1305 [1]
Apparent magnitude  (V)4.47 - 4.54 [2]
Characteristics
Spectral type B2.5V [3]
U−B color index −0.68 [4]
B−V color index -0.20 [4]
Variable type ellipsoidal [2]
Astrometry
Radial velocity (Rv)+29.50 [5]  km/s
Proper motion (μ)RA: −8.92 [1]   mas/yr
Dec.: +3.34 [1]   mas/yr
Parallax (π)5.03 ± 0.19  mas [1]
Distance 650 ± 20  ly
(199 ± 8  pc)
Absolute magnitude  (MV)−2.00 [6]
Details
Mass 6.0 [7]   M
Radius 7.3 [7]   R
Luminosity 2,268 [7]   L
Surface gravity (log g)3.5 [7]   cgs
Temperature 15,254 [7]   K
Metallicity [Fe/H]−0.15 [8]   dex
Rotational velocity (v sin i)151 [9]  km/s
Age 24.1 [10]   Myr
Other designations
b Puppis, QZ Pup, CD−38°3769, GC  10661, GSC  07646-03591, HIP  38455, HR  3084, HD  64503, NSV  3789, SAO  198545
Database references
SIMBAD data

QZ Puppis (QZ Pup, b Pup) is a class B2.5V (blue main-sequence) star in the constellation Puppis. Its apparent magnitude is 4.5 and it is approximately 650 light years away based on parallax.

A light curve for QZ Puppis, plotted from TESS data QZPupLightCurve.png
A light curve for QZ Puppis, plotted from TESS data

QZ Puppis was identified as a small-amplitude variable star in 1974, but the nature of the variability was unclear. It was thought to be a spectroscopic binary on the basis of variability in the radial velocity of its spectral lines. [12] As a hot B-class main sequence star with variable spectral lines, it was suspected of being a β Cephei variable but this classification was repeatedly rejected. [13] The short-period sinusoidal variations in brightness with an amplitude of 0.03 magnitudes were interpreted as ellipsoidal variations as the star, distorted by a close companion, rotates with a period of 1.1 days. [12] Later analysis of Hipparcos photometry detected shallow eclipses. [14]

The companion to QZ Puppis is only known from its effect on the visible star as they orbit. The primary shows radial velocity variations of 71 km/s as it orbits every 1.112 days.

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References

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