TT Arietis: an evolved, very short period binary.
Abstract
A spectroscopic investigation of the rapid variable TT Ari reveals it to be a binary system with an orbital period of 0.1375 days. The spectrum is nearly continuous, with weak hydrogen emission lines superposed on shallow broad absorption. Broad C III and He II emission and narrower He I absorption are present, but very weak. The strength of the H emission is found to vary with the orbital phase, reaching a maximum intensity near quadrature (with the hot primary receding). The presence of a nonuniform, rotating ring surrounding the primary is inferred from the H emission lines. The complex light variations show a broad maximum during each orbital period, in addition to rapid flickering. This variation may be due to a hot spot in a ring or disk around the primary excited by infalling matter from the secondary. The inferred model of the system is similar to that derived for old novae.
- Publication:
-
The Astrophysical Journal
- Pub Date:
- January 1975
- DOI:
- 10.1086/153341
- Bibcode:
- 1975ApJ...195..413C
- Keywords:
-
- Binary Stars;
- Novae;
- Stellar Spectrophotometry;
- Variable Stars;
- Absorption Spectra;
- Astronomical Models;
- Balmer Series;
- Continuous Spectra;
- Emission Spectra;
- H Lines;
- Orbital Elements;
- Stellar Evolution;
- X Ray Astronomy;
- Astrophysics