Period changes in eruptive binaries.
Abstract
The residuals (O-C) of nine binary systems are statistically analyzed for evidence of period changes from which the rate of mass transfer may be deduced. Least square analysis of linear regression is applied to T Aurigae, Z Chamaeleontics, EM Cygni, U Geminorum, DQ Herculis, EX Hydrae, VV Puppis, V Sagittae, and WZ Sagittae; only T Aur and EM Cyg show reasonable evidence for a change of period. It is noted that the period change cannot be determined as monotonic or periodic, and that the relationship between the rate of mass transfer and the period change is entirely dependent on the method of mass loss. It is thus concluded that an accurate estimate of the rate of mass transfer cannot be deduced from a change of binary period.
- Publication:
-
Monthly Notices of the Royal Astronomical Society
- Pub Date:
- March 1975
- DOI:
- 10.1093/mnras/170.3.633
- Bibcode:
- 1975MNRAS.170..633P
- Keywords:
-
- Dwarf Stars;
- Eclipsing Binary Stars;
- Orbital Elements;
- Statistical Analysis;
- Stellar Mass Ejection;
- White Dwarf Stars;
- Mass Transfer;
- Novae;
- Orbit Calculation;
- Spectral Bands;
- Stellar Spectra;
- Variable Stars;
- Astrophysics