Psi Velorum

Psi Velorum, Latinized from ψ Velorum, is a binary star system in the southern constellation of Vela. Based upon an annual parallax shift of 53.15 mas as seen from Earth, it is located 61.4 light years from the Sun. It is visible to the naked eye with a combined apparent visual magnitude of +3.58.^[2] The motion of this system through space makes it a candidate member of the Castor stellar kinematic group.^[11]

Psi Velorum

Location of ψ Velorum
Observation data Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation	Vela
Right ascension	09h 30m 41.99958s[1]
Declination	−40° 28′ 00.2616″[1]
Apparent magnitude (V)	+3.58[2] (3.91 + 5.12)[3]
Characteristics
Evolutionary stage	Main sequence[4] or subgiant[5]
Spectral type	F0 IV + F3 IV[5]
U−B color index	+0.00[2]
B−V color index	+0.36[2]
Astrometry
Radial velocity (Rv)	+8.8±1.8[6] km/s
Proper motion (μ)	RA: −147.98[1] mas/yr Dec.: +61.35[1] mas/yr
Parallax (π)	53.15±0.37 mas[1]
Distance	61.4 ± 0.4 ly (18.8 ± 0.1 pc)
Absolute magnitude (MV)	2.56[7]
Orbit[8]
Period (P)	33.95 yr
Semi-major axis (a)	0.862″
Eccentricity (e)	0.433
Inclination (i)	58.0°
Longitude of the node (Ω)	291.0°
Periastron epoch (T)	1969.68
Argument of periastron (ω) (secondary)	44.3°
Details[9]
ψ Vel A
Mass	1.46 M☉
Radius	1.46[a] R☉
Luminosity	4.21 L☉
Temperature	6,837 K
Metallicity [Fe/H]	0.0±0.2[5] dex
ψ Vel B
Mass	1.34 M☉
Radius	1.54[a] R☉
Luminosity	3.05 L☉
Temperature	6,148 K
Metallicity [Fe/H]	0.0±0.2[5] dex
Other designations
ψ Vel, CD−39°5580, GJ 351, HD 82434, HIP 46651, HR 3786, SAO 221234, WDS J09307-4028AB[10]
Database references
SIMBAD	ψ Vel
	ψ Vel A
	ψ Vel B
ARICNS	ψ Vel A
	ψ Vel B

The two components of this system orbit their common barycenter with a period of 33.95 years and an eccentricity of 0.433. The semimajor axis of their orbit has an angular size of 0.862 arc seconds.^[8] Psi Velorum A and Psi Velorum B have apparent magnitudes of +3.91 and +5.12^[3] and spectral types F0 IV and F3 IV, suggesting they are F-type subgiants.^[5] Analysis of the stars' properties suggest that they are main sequence stars rather than subgiants,^[4] and spectral types of F3V + F have also been published.^[9] The secondary has been reported to be variable between magnitude 4.5 and 5.1.^[12]

Notes

1. Calculated, using the Stefan-Boltzmann law and the stars' effective temperature and luminosity, with respect to the solar nominal effective temperature of 5,772 K:$${\displaystyle {\sqrt {{\biggl (}{\frac {5,772}{6,837}}{\biggr )}^{4}\cdot 4.21}}=1.46\ R_{\odot }.}$$$${\displaystyle {\sqrt {{\biggl (}{\frac {5,772}{6,148}}{\biggr )}^{4}\cdot 3.05}}=1.54\ R_{\odot }.}$$