Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Auriga |
Right ascension | 04h 55m 59.38527s [1] |
Declination | +30° 34′ 01.5190″ [1] |
Apparent magnitude (V) | 9.30 [2] |
Characteristics | |
Spectral type | G2IIIne [2] |
B−V color index | +0.74 [3] |
Variable type | T Tauri |
Astrometry | |
Radial velocity (Rv) | 23.20 [4] km/s |
Proper motion (μ) | RA: 1.18 [1] mas/yr Dec.: -22.24 [1] mas/yr |
Parallax (π) | 6.85 ± 2.23 mas [1] |
Distance | approx. 500 ly (approx. 150 pc) |
Absolute magnitude (MV) | +2.83 [3] |
Details [3] | |
Mass | 2.0±0.1 M☉ |
Radius | 2.61+0.20 −0.23 R☉ |
Luminosity | 6.3±1.6 L☉ |
Surface gravity (log g) | 3.91+0.07 −0.10 cgs |
Temperature | 5550±100 K |
Rotation | 1.76+0.29 −0.33 |
Rotational velocity (v sin i) | 66.2 km/s |
Age | 4 Myr |
Other designations | |
Database references | |
SIMBAD | data |
SU Aurigae is a T Tauri-type variable star in the constellation Auriga. It is located about 500 light-years (150 parsecs) away in the Taurus-Auriga Star Forming Region. Its apparent magnitude is 9.30, which is dim enough that it cannot be seen with the unaided eye.
In 1907, Henrietta Swan Leavitt discovered that SU Aurigae is a variable star. [5]
SU Aurigae's spectral type of G2IIIne means that it is a G-type star with an effective temperature similar to the Sun. The III in the spectral type refers to its luminosity, which is much higher than normal G-type main sequence stars and would put it in the giant star class. [6] However, it is only about 4 million years old, which is relatively young for a star - young protostars like SU Aurigae are luminous because they are larger, not condensing into a normal size until they are older. [7]
SU Aurigae is known to have a circumstellar protoplanetary disk surrounding it, which is typical of many T Tauri stars. [7] SU Aurigae's disk has a high inclination of 62° and is nearly perpendicular to the plane of sky, so orbiting protoplanets or comets may be the cause of why there are drops in the amount of light detected. [3] SU Aurigae's proper motion and distance is similar to AB Aurigae, [1] a better known pre-main-sequence star, meaning that the two may form a very wide binary system; [6] if not, they are still in the same star association.
Telescopium Herschelii, also formerly known as Tubus Hershelli Major, is a former constellation in the northern celestial hemisphere. Maximilian Hell established it in 1789 to honour Sir William Herschel's discovery of the planet Uranus. It fell out of use by the end of the 19th century. θ Geminorum at apparent magnitude 4.8 was the constellation's brightest star.
Iota Aurigae, officially named Hassaleh, is a star in the northern constellation of Auriga. It has an apparent visual magnitude of 2.7, which is bright enough to be readily visible to the naked eye. Parallax measurements give a distance estimate of roughly 490 light-years from the Sun.
Eta Aurigae, officially named Haedus, is a star in the northern constellation of Auriga. With an apparent visual magnitude of 3.18, it is visible to the naked eye. Based upon parallax measurements made during the Hipparcos mission, this star is approximately 243 light-years distant from the Sun.
Pi Aurigae, Latinized from π Aurigae, is the Bayer designation for a single, red-hued star in the northern constellation of Auriga. Located about one degree north of the 2nd magnitude star Beta Aurigae, Pi Aurigae is visible to the naked eye with an apparent visual magnitude of 4.25 Based upon parallax measurements, it is approximately 720 light-years away from Earth. At that distance, the brightness of the star is diminished by 0.54 in magnitude from extinction caused by interstellar gas and dust.
Mu Aurigae, Latinized as μ Aurigae, is the Bayer designation for an unconfirmed binary star in the northern constellation of Auriga. It is visible to the naked eye with an apparent visual magnitude of +4.88. Based upon an annual parallax shift of 20.7218±0.4971 mas as seen from Earth, is located 157 light-years from the Sun.
19 Aurigae is a single star located approximately 3,800 light years away from the Sun in the northern constellation Auriga. It is visible to the naked eye as a faint, white-hued star with an apparent visual magnitude of 5.05. The star is moving closer to the Earth with a heliocentric radial velocity of 4.3 km/s.
Omicron Aurigae, Latinized from ο Aurigae, is the Bayer designation for an astrometric binary star system in the northern constellation of Auriga. With an apparent visual magnitude of 5.47, it is faintly visible to the naked eye. Based upon an annual parallax shift of 7.89 ± 0.84 mas, it is approximately 413 light-years distant from Earth. The star is a member of the Ursa Major stream of co-moving stars.
AE Aurigae is a runaway star in the constellation Auriga; it lights the Flaming Star Nebula.
59 Aurigae, often abbreviated as 59 Aur, is a star in the constellation Auriga. Its baseline apparent magnitude is 6.1, meaning it can just barely be seen with the naked eye as a dim, yellow-white hued star. Based on parallax measurements, it is located about 483 light-years away from the Sun.
AR Aurigae, 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.
Psi4 Aurigae, Latinized from ψ4 Aurigae, is a single, orange-hued star in the northern constellation of Auriga. It is visible to the naked eye with an apparent visual magnitude of +5.02. With an annual parallax shift of 10.08 ± 0.33 mas, it is approximately 324 light-years distant from Earth.
Psi5 Aurigae is a star in the northern constellation of Auriga. It is faintly visible to the naked eye with an apparent visual magnitude of 5.25. Based upon parallax measurements made during the Hipparcos mission, this star is approximately 53.9 light-years distant from Earth. There is an optical companion which is 36 arcseconds away and has an apparent magnitude of +8.4.
Psi8 Aurigae is a star in the northern constellation of Auriga. It has an apparent visual magnitude of 6.443 and, based upon parallax measurements, they are approximately 750 light-years distant from the Earth.
Psi9 Aurigae, Latinised from ψ9 Aurigae, is a star in the northern constellation of Auriga. It is dimly visible to the naked eye with an apparent visual magnitude of 5.75. Based upon an annual parallax shift of 2.59 mas, the distance to this star is approximately 1,300 light-years.
16 Lyncis is a star in the constellation Lynx. It is positioned next to the western constellation border with Auriga, and is also known as Psi10 Aurigae, which is Latinized from ψ10 Auriga. The star has a white hue and is visible to the naked eye with an apparent visual magnitude of 4.90. The distance to this object is approximately 241 light-years based on parallax, but it is drifting closer to the Sun with a radial velocity of −12 km/s. It has an absolute magnitude of 0.56.
IQ Aurigae is a single, variable star in the northern constellation of Auriga. It is visible to the naked eye as a dim, white-hued star with an apparent visual magnitude that fluctuates around 5.38. The star is located at a distance of about 460 light-years from the Sun based on parallax and is drifting further away with a radial velocity of +28.6 km/s.
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.
V433 Aurigae is a variable star in the constellation Auriga. It is a slowly pulsating B star (SPB) that ranges from apparent magnitude 6.02 to 6.06 over 4.6 days. Using a Hipparcos-derived distance of about 1,060 light-years (324 pc), it shines with a luminosity approximately 322 times that of the Sun and has a surface temperature of 7400 K. However, measurements by Gaia indicate a much higher distance of 3,200 light-years (980 pc).
AB Aurigae is a young Herbig Ae star in the Auriga constellation. It is located at a distance of approximately 531 light years from the Sun based on stellar parallax. This pre-main-sequence star has a stellar classification of A0Ve, matching an A-type main-sequence star with emission lines in the spectrum. It has 2.4 times the mass of the Sun and is radiating 38 times the Sun's luminosity from its photosphere at an effective temperature of 9,772 K. The radio emission from the system suggests the presence of a thermal jet originating from the star with a velocity of 300 km s−1. This is causing an estimated mass loss of 1.7×10−8 M☉ yr−1.
RW Aurigae is a young binary system in the constellation of Auriga about 530 light years away, belonging to the Taurus-Auriga association of the Taurus Molecular Cloud. RW Aurigae B was discovered in 1944.