Psi Velorum

Psi Velorum

Location of ψ Velorum
Observation data Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation	Vela
Right ascension	09^h 30^m 41.99958^s[1]
Declination	−40° 28′ 00.2616″[1]
Apparent magnitude (V)	+3.58[2] (3.91 + 5.12)[3]
Characteristics
Spectral type	F0 IV + F3 IV[4]
U−B color index	+0.00[2]
B−V color index	+0.36[2]
Astrometry
Radial velocity (Rv)	+8.8±1.8[5] 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[6]
Orbit[7]
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[8]
ψ Vel A
Mass	1.56[9] M☉
Radius	1.6 R☉
Luminosity	6.0 L☉
Surface gravity (log g)	4.27[10] cgs
Temperature	7,130 K
Metallicity [Fe/H]	0.0±0.2[4] dex
Rotational velocity (v sin i)	156.0[11] km/s
Age	889[10] Myr
ψ Vel B
Mass	~1.5 M☉
Radius	1.2 R☉
Luminosity	3.8 L☉
Temperature	7,400 K
Other designations
ψ Vel, CD−39°5580, GJ 351, HD 82434, HIP 46651, HR 3786, SAO 221234, WDS J09307-4028AB[12]
Database references
SIMBAD	ψ Vel
	ψ Vel A
	ψ Vel B
ARICNS	ψ Vel A
	ψ Vel B

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.[13]

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.[7] The primary, component A, is a yellow-white hued F-type subgiant with an apparent magnitude of +3.91[3] and a stellar classification of F0 IV.[4] The fainter secondary, component B, is also an F-type subgiant of magnitude +5.12[3] and class F3 IV.[4] Analysis of the stars' properties suggest that they are main sequence stars rather than subgiants.[8] It has been reported to be variable between magnitude 4.5 and 5.1.[14]

References

1. van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357, S2CID 18759600.
2. Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data, SIMBAD, Bibcode:1986EgUBV........0M.
3. Malkov, O. Yu.; et al. (2012), "Dynamical Masses of a Selected Sample of Orbital Binaries", Astronomy & Astrophysics, 546: 5, Bibcode:2012A&A...546A..69M, doi:10.1051/0004-6361/201219774, A69.
4. Heiter, U.; et al. (2015), "Gaia FGK benchmark stars: Effective temperatures and surface gravities", Astronomy & Astrophysics, 582: A49, arXiv:1506.06095, Bibcode:2015A&A...582A..49H, doi:10.1051/0004-6361/201526319, S2CID 53391939.
5. de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project", Astronomy & Astrophysics, 546: 14, arXiv:1208.3048, Bibcode:2012A&A...546A..61D, doi:10.1051/0004-6361/201219219, S2CID 59451347, A61.
6. Just, A.; Jahrei, H. (October 2008), "The main sequence from F to K stars of the solar neighbourhood in SDSS colours", Astronomische Nachrichten, 329 (8): 790, arXiv:0808.2111, Bibcode:2008AN....329..790J, doi:10.1002/asna.200811030, S2CID 18793369.
7. Hartkopf, W. I.; et al. (2006), Sixth Catalog of Orbits of Visual Binary Stars, archived from the original on 2011-05-17, retrieved 2017-04-03
8. "Psi Velorum", stars.astro.illinois.edu, retrieved 2025-01-17
9. Fuhrmann, K.; Chini, R.; Kaderhandt, L.; Chen, Z. (2017-02-10), "Multiplicity among Solar-type Stars", The Astrophysical Journal, 836 (1): 139, doi:10.3847/1538-4357/836/1/139, ISSN 0004-637X
10. David, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets", The Astrophysical Journal, 804 (2): 146, arXiv:1501.03154, Bibcode:2015ApJ...804..146D, doi:10.1088/0004-637X/804/2/146, S2CID 33401607.
11. Schröder, C.; Reiners, Ansgar; Schmitt, Jürgen H. M. M. (January 2009), "Ca II HK emission in rapidly rotating stars. Evidence for an onset of the solar-type dynamo" (PDF), Astronomy and Astrophysics, 493 (3): 1099–1107, Bibcode:2009A&A...493.1099S, doi:10.1051/0004-6361:200810377^[permanent dead link‍]
12. "* psi Vel". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-03-31.
13. Nakajima, Tadashi; et al. (September 2010), "Potential Members of Stellar Kinematical Groups within 20 pc of the Sun", The Astronomical Journal, 140 (3): 713–722, Bibcode:2010AJ....140..713N, doi:10.1088/0004-6256/140/3/713.
14. Samus, N. N.; Durlevich, O. V.; et al. (2009), "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)", VizieR On-line Data Catalog: B/gcvs, 1, Bibcode:2009yCat....102025S.