Notes
- 1 2 Calculated, using the Stefan-Boltzmann law and the star's effective temperature and luminosity, with respect to the solar nominal effective temperature of 5,772 K:
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Vela |
| Right ascension | 10h 37m 18.13995s [1] |
| Declination | −48° 13′ 32.2349″ [1] |
| Apparent magnitude (V) | 3.83 [2] (4.13 / 5.76) [3] |
| Characteristics | |
| Spectral type | F3IV + F0V + A6V [2] |
| U−B color index | +0.04 [2] |
| B−V color index | +0.31 [2] |
| Astrometry | |
| Radial velocity (Rv) | 21.20 ± 0.7 [4] km/s |
| Proper motion (μ) | RA: -133.41 [1] mas/yr Dec.: -1.82 [1] mas/yr |
| Parallax (π) | 37.26 ± 0.36 mas [1] |
| Distance | 87.5 ± 0.8 ly (26.8 ± 0.3 pc) |
| Absolute magnitude (MV) | 2.15 / 2.70 / 2.14 [2] |
| Orbit [3] | |
| Primary | p Vel A |
| Companion | p Vel B |
| Period (P) | 16.651 yr |
| Semi-major axis (a) | 0.361″ |
| Eccentricity (e) | 0.726 |
| Inclination (i) | 128.5° |
| Longitude of the node (Ω) | 37.2° |
| Periastron epoch (T) | 2019.562 |
| Argument of periastron (ω) (secondary) | 288.9° |
| Details [5] | |
| p Vel Aa | |
| Mass | 1.88 M☉ |
| Radius | 2.56 [lower-alpha 1] R☉ |
| Luminosity | 12.5 L☉ |
| Temperature | 6,710 K |
| p Vel Ab | |
| Mass | 1.29 M☉ |
| Radius | 1.22 [lower-alpha 1] R☉ |
| Luminosity | 2.79 L☉ |
| Temperature | 6,740 K |
| p Vel B | |
| Mass | 2.41 [2] M☉ |
| Other designations | |
| p Vel A: HD 92139 | |
| p Vel B: HD 92140 | |
| Database references | |
| SIMBAD | data |
p Velorum (abbreviated to p Vel) is a triple star system in the constellation Vela. Parallax measurements by the Hipparcos spacecraft put it at a distance of 87.5 light-years, or 26.8 parsecs from Earth. [1] It is visible to the naked eye with a combined apparent magnitude of 3.83. [2]
The primary component is a spectroscopic binary whose components have an orbital period of 10.21 days. The inner spectroscopic binary consists of two F-type stars, a subgiant and a main-sequence star. [2] There is a companion star which is a white A-type main-sequence star, with an apparent magnitude of 5.76. [3] It is separated 0.361 arcseconds from the primary and has an orbital period of 16.651 years. [3]
Acrux is the brightest star in the southern constellation of Crux. It has the Bayer designation α Crucis, which is Latinised to Alpha Crucis and abbreviated Alpha Cru or α Cru. With a combined visual magnitude of +0.76, it is the 13th-brightest star in the night sky. It is the most southerly star of the asterism known as the Southern Cross and is the southernmost first-magnitude star, 2.3 degrees more southerly than Alpha Centauri. This system is located at a distance of 321 light-years from the Sun.
Beta Arietis, officially named Sheratan, is a star system and the second-brightest star in the constellation of Aries, marking the ram's second horn.
Beta Centauri is a triple star system in the southern constellation of Centaurus. It is officially called Hadar. The Bayer designation of Beta Centauri is Latinised from β Centauri, and abbreviated Beta Cen or β Cen. The system's combined apparent visual magnitude of 0.61 makes it the second-brightest object in Centaurus and the eleventh brightest star in the night sky. According to parallax measurements from the astrometric Hipparcos satellite, the distance to this system is about 390 light-years.
Alpheratz, or Alpha Andromedae, is a binary star 97 light-years from Earth and is the brightest star in the constellation of Andromeda when Mirach undergoes its periodical dimming. Immediately northeast of the constellation of Pegasus, it is the upper left star of the Great Square of Pegasus.
Epsilon Carinae, officially named Avior, is a binary star in the southern constellation of Carina. At apparent magnitude +1.86 it is one of the brightest stars in the night sky, but is not visible from most of the northern hemisphere. The False Cross is an asterism formed of Delta Velorum, Kappa Velorum, Iota Carinae and ε Carinae. It is so called because it is sometimes mistaken for the Southern Cross, causing errors in astronavigation.
R Horologii is a red giant star approximately 760 light-years away in the southern constellation of Horologium. It is a Mira variable with a period of 404.83 days, ranging from apparent magnitude 4.7 to 14.3—one of the largest ranges in brightness known of stars in the night sky visible to the unaided eye. The star is losing mass at the rate of 5.9×10−7 M☉·y−1.
Psi1 Aurigae is a star in the northern constellation of Auriga. It is faintly visible to the naked eye with an apparent visual magnitude of 4.91. Based upon a measured annual parallax shift of 0.44 mas, it is approximately 7,500 light-years distant from the Earth. It is receding from the Sun with a radial velocity of +4.7 km/s.
Iota Centauri, Latinized from ι Centauri, is a star in the southern constellation of Centaurus. Based upon parallax measurements, it lies at a distance of approximately 58.6 light-years from Earth. Iota Centauri has an apparent visual magnitude of +2.73, making it easily visible to the naked eye.
AB Doradus is a pre-main-sequence quadruple star system in the constellation Dorado. The primary is a flare star that shows periodic increases in activity.
R Lyrae, also known as its Flamsteed designation 13 Lyrae, is a 4th magnitude semiregular variable star in the constellation Lyra, approximately 350 light years away from Earth. It is a red giant star of the spectral type M5III, currently at the last stages of evolution. It is much larger and brighter, yet cooler, than the Sun. In the near-infrared J band, it is brighter than the nearby Vega.
HD 33579 is a white/yellow hypergiant and one of the brightest stars in the Large Magellanic Cloud (LMC). It is a suspected variable star.
Sigma Cygni, Latinised from σ Cygni, is a blue supergiant star in the constellation Cygnus. Its apparent magnitude is 4.2. It belongs to the Cygnus OB4 stellar association and is located approximately 3,300 light years away from Earth.
U Hydrae is a single star in the equatorial constellation of Hydra, near the northern constellation border with Sextans. It is a semiregular variable star of sub-type SRb, with its brightness ranging from visual magnitude (V) 4.7 to 5.2 over a 450-day period, with some irregularity. This object is located at a distance of approximately 680 light years from the Sun based on parallax. It is drifting closer with a radial velocity of −26 km/s.
PZ Cassiopeiae is a red supergiant star located in the constellation of Cassiopeia, and a semi-regular variable star.
10 Ursae Majoris is a binary star system in the northern constellation of Lynx. It is visible to the naked eye as a faint star with a combined apparent visual magnitude of 3.960. This system is fairly close to the Sun, at 53 light-years (16.1 pc) away from Earth. It is the third-brightest object in Lynx. Originally in the neighbouring constellation Ursa Major, it became part of Lynx with the official laying down of the constellation borders. The system is moving further from the Earth with a heliocentric radial velocity of 26.4 km/s. It is a probable member of the Hyades supercluster.
Beta Phoenicis is a binary star in the constellation Phoenix. Its apparent magnitude is 3.30, meaning that it can be seen with the naked eye (see Bortle scale).
3 Puppis is a supergiant star in the constellation Puppis. It is a very rare A[e] supergiant, referred to as a B[e] star despite its spectral classification, and its apparent magnitude is 3.93.
TW Horologii is a carbon star and semiregular variable in the southern constellation of Horologium, near the eastern constellation border with Reticulum. It has a ruddy hue and, with an apparent visual magnitude that ranges from 5.52 down to 5.95, is visible to the naked eye and one of the brightest carbon stars. Based on parallax measurements, it is located at a distance of approximately 1,370 light years from the Sun. It is drifting further away with a radial velocity of +14 km/s. In the past this star has been considered a member of the open cluster NGC 1252, but this now seems unlikely.
BC Cygni is a red supergiant and pulsating variable star of spectral type M3.5Ia in the constellation Cygnus.
S Scuti is a carbon star located in the constellation Scutum. Parallax measurements by Hipparcos put it at a distance of approximately 1,300 light-years. Its apparent magnitude is 6.80, making it not quite bright enough to be seen with the naked eye.
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