期刊
ASTRONOMY & ASTROPHYSICS
卷 394, 期 1, 页码 137-149出版社
EDP SCIENCES S A
DOI: 10.1051/0004-6361:20021105
关键词
stars : emission-linel, Be; stars : activity; stars : individual : 66 Oph; stars : oscillations; stars : magnetic field
66 Oph is a Be star seen under a moderate inclination angle that shows strong variability from UV to IR wavelengths. A concise review of long-term variability history is given. High resolution, high S/N spectroscopic observations obtained in 1997, 1998 and 2001 and spectropolarimetric observations obtained in 2000 are presented. These observations occurred during a long-term decrease of Halpha intensity. Fundamental parameters of the star have been revisited from Barbier-Chalonge-Divan (BCD) calibrations. New V sin i values are obtained using Fourier transforms applied to observed helium lines and a rotational frequency f(rot) = 1.29 cd(-1) is determined. Time series analysis and Fourier Doppler Imaging (FDI) of He I lines (4713, 4921, 5876 and 6678 Angstrom) lead for the first time to the detection of multi-periodicity in 66 Oph. The two main frequencies found are f = 2.22 c d(-1) and f = 4.05 c d(-1). They are attributed to non-radial pulsations and can be associated with mode degree l = 2 and l = 3, respectively. Inspection of Stokes V profiles suggests the presence of a weak Zeeman signature but further observations are needed to confirm the detection of a magnetic field in 66 Oph.
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