Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Auriga |
Right ascension | 05h 18m 18.896s [2] |
Declination | +33° 46′ 02.52″ [2] |
Apparent magnitude (V) | 6.144 [3] |
Characteristics | |
Spectral type | B9V + B9.5V [4] |
U−B color index | −0.18 [5] |
B−V color index | −0.06 [5] |
Variable type | Algol [6] |
Astrometry | |
Radial velocity (Rv) | 25.4±0.9 [7] km/s |
Proper motion (μ) | RA: +15.254 [2] mas/yr Dec.: −29.225 [2] mas/yr |
Parallax (π) | 7.0735 ± 0.0461 mas [2] |
Distance | 461 ± 3 ly (141.4 ± 0.9 pc) |
Absolute magnitude (MV) | 1.11/1.17 [8] |
Details | |
AR Aur A | |
Mass | 2.552±0.008 [4] M☉ |
Radius | 1.781 [9] R☉ |
Luminosity | 41 [8] L☉ |
Surface gravity (log g) | 4.33 [4] cgs |
Temperature | 10,950±150 [4] K |
Rotational velocity (v sin i) | 10 [9] km/s |
AR Aur B | |
Mass | 2.367±0.008 [4] M☉ |
Radius | 1.816 [9] R☉ |
Luminosity | 34 [8] L☉ |
Surface gravity (log g) | 4.28 [4] cgs |
Temperature | 10,350±150 [4] K |
Rotational velocity (v sin i) | 11 [9] km/s |
Other designations | |
Database references | |
SIMBAD | data |
AR Aurigae (AR Aur), also known by its Flamsteed designation 17 Aurigae, is a binary star in the constellation Auriga. Based on parallax measurements made by the Hipparcos spacecraft, it is approximately 461 light-years from Earth. [10]
Both components are blue-white B-type main-sequence stars that do not fill their Roche lobes. The system has a mean apparent magnitude of +6.15. However, the orbit of the stars are oriented in such a way that they periodically eclipse each other, so AR Aurigae is a variable star and its brightness varies from magnitude +6.15 to +6.82 with a period of 4.13 days. [6]
The primary component of AR Aurigae is known to be a mercury-manganese star, also known as an HgMn star. As the name implies, these stars have over-abundances of the elements mercury and manganese, and also often xenon and other elements. [4] Because AR Aurigae is an eclipsing binary (in fact, it is the only known eclipsing binary with a mercury-manganese star), accurate characterization of its parameters has been made possible. Based on the light-time effect observed from the stars, it is inferred that there is a third star with a mass of 0.54 M☉, orbiting at a separation of 13 au every 23.7 years. [4]
26 Andromedae, abbreviated 26 And, is a binary star system in the constellation Andromeda. 26 Andromedae is the Flamsteed designation. It has a combined apparent visual magnitude of 6.10, which is near the lower limit of visibility to the naked eye. The distance to this system can be estimated from its annual parallax shift of 5.35 mas, which yields a distance of about 600 light years. At that distance, the visual magnitude of the stars is diminished from an extinction of 0.04 due to interstellar dust. The system is moving further from the Earth with a heliocentric radial velocity of +3.3 km/s.
74 Aquarii is a triple star system in the constellation of Aquarius. 74 Aquarii is its Flamsteed designation and it also bears the variable star designation HI Aquarii. The combined apparent visual magnitude is 5.8, although it is very slightly variable, and it is located at a distance of 590 light-years from Earth.
9 Aurigae is a star system in Auriga (constellation). It has an apparent magnitude of about 5, making it visible to the naked eye in many suburban skies. Parallax estimates made by the Hipparcos spacecraft put it at about 85.7 light-years from the solar system.
RT Aurigae is a yellow supergiant variable star in the constellation Auriga, about 1,500 light years from Earth.
53 Aurigae is a binary star system in the northern constellation of Auriga. It is visible to the naked eye as a dim star with a combined apparent visual magnitude of 5.74. Parallax estimates put it at a distance of 383 light-years away. The system is receding from the Earth with a heliocentric radial velocity of 13 km/s.
AE Aurigae is a runaway star in the constellation Auriga; it lights the Flaming Star Nebula.
PU Aurigae is an irregular variable star located in the constellation Auriga. A red giant, it varies by 0.1 magnitude around magnitude 5.64. Located around 560 light-years distant, it shines with a luminosity approximately 1,523 times that of the Sun and has a surface temperature of 3,482 K.
IU Aurigae is a triple star system in the constellation Auriga, consisting of an eclipsing binary pair orbiting a third component with a period of 335 years. This system is too faint to be viewed with the naked eye, having a peak apparent visual magnitude of 8.19. The eclipsing pair form a Beta Lyrae-type semidetached binary of two Bp stars with a period of 1.81147435 days. During the primary eclipse, the visual magnitude of the system drops to 8.89, while for the secondary it decreases to 8.74. The third component is a massive object with 17–18 M☉, and may actually be a binary – which would make this a quadruple star system.
LY Aurigae is a multiple star system in the constellation Auriga. It is an eclipsing binary variable star, dropping in brightness by 0.7 magnitudes every 4 days. The system is around a thousand light years away in the Auriga OB1 stellar association.
YZ Cassiopeiae is a star system 103.8 parsecs (339 ly) away from Earth, in the constellation Cassiopeia. It comprises three stars: an eclipsing Algol-type binary and a visually fainter star about 3000 AU distant.
NO Aurigae is a pulsating variable star in the constellation Auriga. It is an unusually-luminous asymptotic giant branch star about 3,500 light years away.
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.
Tau Persei, also known as 18 Persei, is a binary star in the constellation of Perseus. The system is fairly close, and is located about 254 light-years away, based on its parallax.
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.
1 Persei is an eclipsing binary star in the constellation Perseus. Its uneclipsed apparent magnitude is 5.49. The binary star consists of two B2 type main-sequence stars in a 25.9 day eccentric orbit. The stars are surrounded by a faint cloud of gas visible in mid-infrared, although whether they are the origin of the gas or simply passing through it is unclear.
31 Cygni, also known as ο1 Cygni, Omicron1 Cygni, or V695 Cygni, is a triple star system about 750 light years away in the constellation Cygnus.
V3903 Sagittarii is an eclipsing binary star system in the constellation Sagittiarus. It creates an H II region LBN 29 1,070 parsecs away from the Sun.
ZZ Boötis is a star system in the constellation Boötes. It varies from magnitude 6.79 to 7.44 over five days. Based on its parallax, measured by the Gaia spacecraft, it is about 350 light-years away.
CD Crucis, also known as HD 311884, is an eclipsing binary star system in the constellation Crux. It is around 14,000 light years away near the faint open cluster Hogg 15. The binary contains a Wolf–Rayet star and is also known as WR 47.
HR 7484 is a binary star system in the northern constellation of Cygnus. It is dimly visible to the naked eye under good viewing conditions, having an apparent visual magnitude of 5.89. Based upon an annual parallax shift of 24.71, it is located 132 light years away. The system is moving closer with a heliocentric radial velocity of −14 km/s.