T Aurigae

Not to be confused with Tau Aurigae.
T Aurigae

RGB composite color image of the shell surrounding the nova T Aurigae, made from three narrow band images: Blue = 4800Å, green = Hα at 6563 Å and red = [NII] at 6583 Å. From Santamaria et al. 2020[1]
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Auriga
Right ascension 05h 31m 59.118s[2]
Declination +30° 26′ 45.03″[2]
Apparent magnitude (V) 4.5Max.
15Min.
Astrometry
Distance880+46
−35[3] pc
Characteristics
Variable type Classical Nova, Eclipsing Binary
Other designations
Nova Aur 1891, GCRV 56251, Lan 652, SBC9 326, BD+30° 923a, HD 36294, CDS 507, HR 1841, AAVSO 0525+30, Gaia DR2 3446266197646225536
Database references
SIMBADdata
Location of T Aurigae (circled in red)

T Aurigae (or Nova Aurigae 1891) was a nova, which lit up in the constellation Auriga in 1891. Thomas David Anderson, an amateur astronomer in Edinburgh, reported that he was "almost certain" he saw the nova at 02:00 UT on 24 January 1892, when it was slightly brighter than χ Aurigae (apparent magnitude 4.74). He mistook the star for 26 Aurigae, although he noted to himself that it seemed brighter than he remembered it being. He saw it twice more during the following week. On 31 January 1892 he realized his mistake, and wrote a note to Ralph Copeland (the Astronomer Royal of Scotland) reporting his discovery.[4] Professor Copeland immediately reported the discovery via telegram to William Huggins, who made the first spectroscopic observations of T Aurigae on 2 February 1892, when the star was a magnitude 4.5 object.[5] T Aurigae was the first nova to be observed spectroscopically.[6]

The light curve of T Aurigae, plotted from photographic magnitude data tabulated by Shapley.[7] Data values listed with identical times were averaged before being plotted.

Strope and Schaefer report that the peak brightness of T Aurigae was magnitude 4.5,.[8] Pre-discovery images on photographic plates allowed the a light curve beginning in late 1891 to be constructed.[7] AAVSO data shows that T Aurigae's quiescent magnitude is 15.3.

In 1958 observations of the stars forming T Aurigae with the Crossley telescope showed that it is an eclipsing binary, with a period of 4.9 hours, and an eclipse depth of 0.18 magnitudes.[9] T Aurigae was the third nova that was discovered to be a short-period eclipsing binary, and that discovery led to increased speculation that the nova phenomenon was connected to close binary star pairs.[10] Today it is believed that all novae are binary stars, with a "donor" star orbiting a white dwarf. The stars are so close to each other that matter is transferred from the donor star to the white dwarf.

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