Astronomy and Astrophysics – Astrophysics
Scientific paper
Nov 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009a%26a...506.1319r&link_type=abstract
Astronomy and Astrophysics, Volume 506, Issue 3, 2009, pp.1319-1333
Astronomy and Astrophysics
Astrophysics
3
Stars: Early-Type, Binaries: Spectroscopic, Stars: Emission-Line, Be, Stars: Individual: Ζ Tauri
Scientific paper
Context: One way to understand the still mysterious Be phenomenon is to study the time variations of particular Be stars with a long observational history. ζ Tau is one obvious candidate. Aims: Using our rich series of spectral and photometric observations and a critical compilation of available radial velocities, spectrophotometry of Hα, and UB{}V photometry, we characterize the pattern of time variations of ζ Tau over about a century. Our goal is to find the true timescales of its variability and confront them with the existing models related to various aspects of the Be phenomenon. Methods: Spectral reductions were carried out using the IRAF and SPEFO programs. The HEC22 program was used for both photometric reductions and transformations to UB{}V. Orbital solutions were derived with the latest publicly available version of the program FOTEL, period analyses employed both the PDM and Fourier techniques - programs HEC27 and PERIOD04. Results: We derived a new orbital ephemeris TRV max.= HJD (2447025.6±1.8) + (132^d.987 ±0^d.050) × E. The analysis of long-term spectral and light variations shows a clear correlation between the RV and V/R changes, and a very complex behaviour of the light changes. The character of the orbital light and V/R changes varies from season to season.
Based on new spectral and photometric observations from the following observatories: Dominion Astrophysical Observatory, Fairborn, Haute Provence, Hvar, Limber, McDonald, Ondřejov, and Ritter.
Appendices are only available in electronic form at http://www.aanda.org
Bjorkman Karen
Bozic Hrvoje
Chadima Pavel
Firt Roman
Gies Douglas R.
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