Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Orion |
Right ascension | 05h 40m 50.71498s [1] |
Declination | −01° 07′ 43.6366″ [1] |
Apparent magnitude (V) | 4.95 [2] |
Characteristics | |
primary | |
Spectral type | B3V [3] |
U−B color index | −0.83 [4] |
B−V color index | −0.21 [4] |
secondary | |
Spectral type | B1 [5] |
Astrometry | |
Radial velocity (Rv) | +26.10 [6] km/s |
Proper motion (μ) | RA: −1.50 [1] mas/yr Dec.: −0.84 [1] mas/yr |
Parallax (π) | 3.63 ± 0.37 mas [1] |
Distance | approx. 900 ly (approx. 280 pc) |
Absolute magnitude (MV) | −2.74 [2] |
Orbit [7] | |
Period (P) | 27.154925 d |
Eccentricity (e) | 0.739±0.007 |
Periastron epoch (T) | 2447886.076±0.065 HJD |
Argument of periastron (ω) (secondary) | 81.4±2.4° |
Semi-amplitude (K1) (primary) | 84.7±1.1 km/s |
Details | |
A | |
Mass | 8.6±0.2 [8] M☉ |
Radius | 5.3 [9] R☉ |
Luminosity | 4,830 [10] L☉ |
Surface gravity (log g) | 3.84 [9] cgs |
Temperature | 21,150 [10] K |
Metallicity [Fe/H] | +0.01 [11] dex |
Rotational velocity (v sin i) | 75 [12] km/s |
Age | 18.0±3.2 [8] Myr |
B | |
Mass | 8.3 [5] M☉ |
Other designations | |
Database references | |
SIMBAD | data |
HD 37756 is a binary star system in the equatorial constellation of Orion, positioned less than a degree to the north of the bright star Alnitak. [14] It has a blue-white hue and is faintly visible to the naked eye with an apparent visual magnitude of 4.95. [2] The system is located at a distance of approximately 900 light years from the Sun based on parallax, [1] and is drifting further away with a radial velocity of +26 km/s. [6] It is a member of the OB1b subgroup of the Orion OB1 association. [15]
The binary nature of this system was identified by E. B. Frost in 1904. [16] It is a double-lined spectroscopic binary with an orbital period of 27.15 days and a high eccentricity of 0.74. [7] The spectrum matches a massive B-type main-sequence star with a stellar classification of B3V. [3] The secondary is luminous enough to interfere with measurements of the primary spectrum. [16] It is a suspected Cepheid variable with a period of 0.37968 days and an amplitude of 0.03 magnitude in the B band of the UBV photometric system. [17] The system is a candidate eclipsing binary with a minimum dip of 0.04 in visual magnitude during each orbit. [18]
Tau Tauri, Latinized from τ Tauri, is a quadruple star system in the constellation Taurus. It is visible to the naked eye as a faint point of light with a combined apparent visual magnitude of 4.33. The distance to this system is approximately about 400 light years based on parallax. The system is moving further from the Earth with a heliocentric radial velocity of +14.6 km/s, and it is a member of the Taurion OB association, located between Orion and Taurus. It is located 0.7 degree north of the ecliptic, and thus is subject to lunar occultations.
2 Andromedae, abbreviated 2 And, is a binary star system in the northern constellation of Andromeda. 2 Andromedae is the Flamsteed designation. It is a faint star system but visible to the naked eye with a combined apparent visual magnitude of 5.09. Based upon an annual parallax shift of 7.7 mas, it is located 420 light years away. The binary nature of the star was discovered by American astronomer Sherburne Wesley Burnham at Lick Observatory in 1889. The pair orbit each other over a period of 74 years with a high eccentricity of 0.8.
36 Andromedae is a visual binary star system in the northern constellation of Andromeda. The designation is from the star catalogue of English astronomer John Flamsteed, first published in 1712. It is faintly visible to the naked eye with an apparent visual magnitude of 5.45. An annual parallax shift of 26.33 mas yields a distance estimate of about 124 light years. The system is moving closer to the Sun with a radial velocity of −0.8 km/s.
Pi2 Cygni, Latinized from π2 Cygni, is a triple star system in the northern constellation of Cygnus. It is visible to the naked eye about 2.5° east-northeast of the open cluster M39, having an apparent visual magnitude of 4.24. Based upon an annual parallax shift of 2.95 mas, it is located at a distance of roughly 1,100 light years from the Sun.
13 Vulpeculae is a blue giant with a stellar classification of class B9.5III in the northern constellation Vulpecula. It is visible to the naked eye as a faint, blue-white hued star with an apparent visual magnitude of 4.57 and it is approximately 339 light years away from the Sun based on parallax. The star is radiating 180 times the luminosity of the Sun from its photosphere at an effective temperature of 8,801 K.
Pi Cephei is a trinary star located in the constellation Cepheus. With a combined apparent magnitude of about 4.4, the system is faintly visible to the naked eye. The inner pair of stars orbits in 1.5 years while the outer companion completes one orbit in about 160 years.
V381 Cephei is a triple star system in the northern constellation of Cepheus. Its apparent magnitude is slightly variable between 5.5 and 5.7.
μ Cygni, Latinised as Mu Cygni, is a binary star system in the northern constellation of Cygnus. It is visible to the naked eye as a faint point of light with a combined apparent visual magnitude of 4.49. The system is located 72 light years distant from the Sun, based on parallax, and is drifting further away with a radial velocity of +17 km/s.
b Persei is a spectroscopic triple star in the constellation Perseus. Its apparent magnitude is 4.60, and it is about 320 light years away.
32 Orionis is a triple star system in the equatorial constellation of Orion. It has the Bayer designation A Orionis, while 32 Orionis is the Flamsteed designation. This system is visible to the naked eye as a faint point of light with a combined apparent visual magnitude of 4.20. It is located approximately 303 light-years away from the Sun based on parallax, and is drifting further away with a radial velocity of +18.6 km/s.
22 Orionis is a binary star in the equatorial constellation of Orion. It has the Bayer designation o Orionis, while 22 Orionis is the Flamsteed designation. This system is visible to the naked eye as a faint, blue-white hued star with an apparent visual magnitude of 4.74. It is located approximately 1,100 light years away from the Sun based on parallax. The system is moving further from the Earth with a heliocentric radial velocity of +28.80
HD 44131 is a star in the equatorial constellation of Orion, positioned near the eastern constellation border with Monoceros. It has a reddish hue and is faintly visible to the naked eye with an apparent visual magnitude of 4.91. The star is located at a distance of approximately 465 light years from the Sun based on parallax, and it is drifting further away with a radial velocity of +48.6 km/s. Based on radial velocity variations, it is a candidate spectroscopic binary system and a preliminary orbital solution was published in 1991 with a period of 9.29 yr. However, these velocity variations may be due to other causes.
78 Pegasi is a binary star system in the northern constellation of Pegasus. It is visible to the naked eye as a faint, orange-hued point of light with an apparent visual magnitude of 4.93. The system is located approximately 224 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −8 km/s. The double-star nature of this system was discovered by A. G. Clark in 1862. The components of this system orbit each other over a 630-year period with an eccentricity of 0.11.
72 Pegasi is a binary star system in the northern constellation of Pegasus. It is visible to the naked eye as a faint, orange-hued point of light with a combined apparent visual magnitude of 4.97. The system is located approximately 550 light years away from the Sun, based on parallax, but is drifting closer with a radial velocity of −25 km/s.
HD 21278 is a binary star system in the constellation Perseus, located within the 60±7 million year old Alpha Persei Cluster. It has a blue-white hue and is visible to the naked eye with a combined apparent visual magnitude of 4.99. The system is located at a distance of approximately 580 light years from the Sun based on parallax, and it is drifting further away with a radial velocity of +1.20 km/s.
HD 69142 is a class K1II-III star in the constellation Puppis. Its apparent magnitude is 4.44 and it is approximately 298 light years away based on parallax.
QZ Puppis is a class B2.5V star in the constellation Puppis. Its apparent magnitude is 4.5 and it is approximately 650 light years away based on parallax.
HD 61330 is a class B8IV star in the constellation Puppis. Its apparent magnitude is 4.53 and it is approximately 360 light years away based on parallax.
HD 64740 is a single star in the southern constellation Puppis, positioned near the line of sight to the Gum Nebula. It has a blue-white hue and is faintly visible to the naked eye with an apparent visual magnitude of 4.63. Parallax measurements give a distance estimate of approximately 760 light-years from the Sun, and it is drifting further away with a radial velocity of +8 km/s.
HD 54893, often called A Puppis is a suspected variable star in the constellation Puppis. Its apparent magnitude is 4.83 and is approximately 860 light years away based on parallax.