Cloud. RW Aurigae B was discovered in 1944. The two stars of the RW Aurigae system are separated by 1.448″, equivalent to 237 AU at the distance of RW Aurigae...

Aurigae". Astronomy and Astro-Physics. 11: 571–581. Bibcode:1892AstAp..11..571H. SIMBAD Psi1 Aurigae. SIMBAD RT Aurigae. SIMBAD RX Aurigae. SIMBAD RW...

average absolute magnitude of +6.55. The object was first suspected to be a RW Aurigae-type star since 1949. It was categorized as a T-Tauri star in 1975. In...

RW Persei is a eclipsing binary star system in the northern constellation of Perseus. It has a peak apparent visual magnitude of 9.68, so this system is...

Bibcode:1975MmSAI..46...81R. Gotz, W. (1961). "Photographische Untersuchungen an RW Aurigae-Sternen in den Dunkelgebieten von Taurus und Orion". Veroeffentlichungen...

C. Hoffmeister in 1949. Hoffmeister classified it as a member of the RW Aurigae-like variables with a brightness that ranged from an apparent visual magnitude...

Tracy L.; Simon, M. (2001), "The Variability of T Tauri, RY Tauri, and RW Aurigae from 1899 to 1952", The Astronomical Journal, 122 (1): 413–417, arXiv:astro-ph/0104268...

segregated it and the similar V533 Centauri as RW Aurigae stars. In time it became clear that RT TrA was unrelated to RW Aur, instead being a member of a group...

et al. (2010). "Infrared images of the transiting disk in the Epsilon Aurigae system". Nature. 464 (7290): 370–2. arXiv:1004.2464. Bibcode:2010Natur...

supernovae Variable star A higher magnitude means a lower brightness. i.e. T Aurigae (+3.8) was a brighter nova than HR Lyrae (+6.5) Prialnik, Dina. "Novae"...