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Epsilon Aurigae

Epsilon Aurigae
Location of ε Aurigae (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Auriga
Right ascension 05h 01m 58.129s[1]
Declination +43° 49′ 23.87″[1]
Apparent magnitude (V) 2.92 - 3.83[2]
Characteristics
Spectral type F0 Iab (or II-III[3]) + ~B5V
U−B color index +0.30[4]
B−V color index +0.54[4]
Variable type Algol[5]
Astrometry
Radial velocity (Rv)−10.40[6] km/s
Proper motion (μ) RA: −0.86±1.38[1] mas/yr
Dec.: −2.66±0.75[1] mas/yr
Parallax (π)0.9879 ± 0.1792 mas[7]
Distance3,642±603 ly
(1,062±185 pc)[8]
Absolute magnitude (MV)-9.1[9]
Orbit[10]
Period (P)9896.0±1.6 d
Semi-major axis (a)18.1+1.2
−1.3[3] AU
Eccentricity (e)0.227±0.011
Inclination (i)89[3]°
Longitude of the node (Ω)264°
Periastron epoch (T)MJD 34723±80
Argument of periastron (ω)
(secondary)		39.2±3.4°
Semi-amplitude (K1)
(primary)		13.84±0.23 km/s
Details
ε Aur A
Mass2.2-15[11] M☉
Radius143 – 358[12] R☉
Luminosity (bolometric)37,875[13] L☉
Surface gravity (log g)≲ 1.0[3] cgs
Temperature7,750[3] K
Rotational velocity (v sin i)54[14] km/s
ε Aur B
Mass6 – 14[11] M☉
Radius3.9±0.4[3] R☉
Surface gravity (log g)4.0[3] cgs
Temperature15,000[3] K
Other designations
Almaaz, Al Anz, ε Aur, 7 Aur, BD+43°1166, FK5 183, HD 31964, HIP 23416, HR 1605, SAO 39955[15]
Data sources:
Hipparcos Catalogue,
Bright Star Catalogue (5th rev. ed.),
9th Catalog of Spectroscopic Binary Orbits,
Variable Star Index (VSX)
Database references
SIMBADdata

Epsilon Aurigae (ε Aurigae, abbreviated Epsilon Aur, ε Aur) is a multiple star system in the northern constellation of Auriga, the charioteer. It is an unusual eclipsing binary system comprising an F0 supergiant (officially named Almaaz /ælˈmɑːz/, the traditional name for the system) and a companion which is generally accepted to be a huge dark disk orbiting an unknown object, possibly a binary system of two small B-type stars. The distance to the system is still a subject of debate, but data from the Gaia spacecraft puts its distance at around 1,350±300 light years from Earth.

Epsilon Aurigae was first suspected to be a variable star when German astronomer Johann Heinrich Fritsch observed it in 1821. Later observations by Eduard Heis and Friedrich Wilhelm Argelander reinforced Fritsch's initial suspicions and attracted attention to the star. Hans Ludendorff, however, was the first to study it in great detail. His work revealed that the system was an eclipsing binary variable, a star that dims when its partner obscures its light.

About every 27 years, Epsilon Aurigae's brightness drops from an apparent visual magnitude of +2.92 to +3.83. This dimming lasts 640–730 days. In addition to this eclipse, the system also has a low amplitude pulsation with a non-consistent period of around 66 days.

Epsilon Aurigae's eclipsing companion has been subject to much debate since the object does not emit as much light as is expected for an object its size. As of 2008, the most popularly accepted model for this companion object is a binary star system surrounded by a massive, opaque disk of dust; theories speculating that the object is a large, semitransparent star or a black hole have since been discarded.

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  7. ^ Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
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