Pi Lupi

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Template:Short description

π Lupi
File:PiLupLightCurve.png
A light curve for Pi Lupi, adapted from Sharma et al. (2022)[1]
Observation data
Epoch J2000      Equinox J2000
Constellation Lupus
Right ascension Template:RA[2]
Declination Template:DEC[2]
Apparent magnitude (V) 3.89[3]
Characteristics
Spectral type B5V + B5IV[4]
U−B Template:Engvar −0.59[3]
B−V Template:Engvar −0.14[3]
Astrometry
Radial velocity (Rv)+4.50[5] km/s
Proper motion (μ) RA: −22.98[2] mas/yr
Dec.: −22.81[2] mas/yr
Parallax (π)7.36±0.55 mas[2]
DistanceTemplate:Rnd ± Template:Rnd ly
(Template:Rnd ± Template:Rnd pc)
Details
A
Mass4.5[6] Template:Solar mass
Surface gravity (log g)4.5[6] cgs
Temperature16,000[6] K
Rotational velocity (v sin i)10[6] km/s
B
Mass4.7[6] Template:Solar mass
Temperature14,000[6] K
Metallicity [Fe/H]{{{metal_fe2}}} dex
Rotational velocity (v sin i)10[6] km/s
Age14[6] Myr
Other designations
CD−46°9773, HIP 73807, SAO 225426
π Lupi A: HD 133242, HR 5605
π Lupi B: HD 133243, HR 5606
Database references
SIMBADdata
A
B

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π Lupi (Latinised to Pi Lupi) is a multiple star system in the southern constellation Lupus. Two components form a wide binary pair with an orbital period of 517 years and a semimajor axis of 1.59″. They belong to the Upper Centaurus Lupus component of the Sco–Cen complex.[4]

At least one of the components is a spectroscopic binary and produces eclipses 15.5 days apart, making it an eclipsing binary. There are also other brightness variations with a period of 16 hours that are likely to be pulsations of the Slowly pulsating B-type star. The eclipses are shallow, with the brightness dropping by only 1% or about 0.01 magnitudes. The amplitude of the pulsations is even smaller.[1]

π Lupi A (HR 5605, HD 133242) has been classified as a spectroscopic binary by at least two studies,[7][8] but both components may be spectroscopic binaries.[9]

References

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Template:Stars of Lupus