Nova T Aurigae 1891: a New Short-Period Eclipsing Binary.
Abstract
Photoelectric observations of T Aur in 1958, 1961, and 1962 indicate that this star is an eclipsing binary with a period of 4h54 Primary eclipse is partial, 0 18 mag. deep, and usually lasts about 40 minutes. No secondary eclipse is observed. The light-curve is of the Algol type and has many features in common with the light-curves of Nova DQ Her, Nova WZ Sge, UX UMa, and RW Tri These similarities include the shortness of the period, bright shoulders before and sometimes after eclipse, asymmetry of the rising branch of the eclipse-curve, and intrinsic variations outside eclipse. The eclipse-curve has no geometrical solution. The discovery of the binary nature of T Aur brings to three the number of extremely short-period eclipsing variables known among the old novae and suggests that the nova phenomenon is most probably related to the binary nature of the stars involved.
- Publication:
-
The Astrophysical Journal
- Pub Date:
- August 1963
- DOI:
- 10.1086/147646
- Bibcode:
- 1963ApJ...138..313W