29 frequencies for the δ Scuti variable BI CMi: the 1997–2000 multisite campaigns |
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| Authors: | M Breger R Garrido G Handler MA Wood RR Shobbrook KM Bischof F Rodler R O Gray A Stankov P Martinez D O'Donoghue R Szabó W Zima A B Kaye C Barban U Heiter |
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| Institution: | 1Astronomisches Institut der Universität Wien, Türkenschanzstr. 17, A–1180 Wien, Austria;2Instituto de Astrofisica de Andalucia, CSIC, Apdo. 3004, E-18080 Granada, Spain;3SAAO, PO Box 9, Observatory 7935, Cape Town, South Africa;4Department of Physics and Space Sciences &SARA Observatory, Florida Institute of Technology, Melbourne, FL 32901, USA;5Department of Physics, University of Sydney, Australia;6Department of Physics and Astronomy, Appalachian State University, Boone, NC 28608, USA;;7Konkoly Observatory, PO Box 67, H-1525 Budapest XII, Hungary;8Applied Physics Division, X-5, Los Alamos National Laboratory, Mail Stop F-663, Los Alamos, NM 87545, USA;9Observatoire de Paris, DASGAL, UMR 8633, 92105 Meudon, France;10National Solar Observatory, 950 N. Cherry, Tucson, AZ 85719, USA |
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| Abstract: | A multisite campaign of BI CMi was carried out with excellent frequency resolution and high photometric accuracy from 1997 to 2000, including two long observing seasons. 29 pulsation frequencies could be extracted from the 1024 h (177 nights) of photometry used. The detected frequencies include 20 pulsation modes in the main pulsation frequency range from 4.8 to 13.0 cycle d−1 (55 to 150 μHz), eight linear combinations of these frequencies, and a very low frequency at 1.66 cycle d−1. Since the value of the low frequency at 1.66 cycle d−1 cannot be identified with a linear combination of other frequencies, g-mode pulsation is suspected, but rotational modulation of abundance spots cannot be ruled out. BI CMi, which is situated near the cool edge of the classical instability strip, may be both a δ Scuti and a γ Doradus star. Another outstanding property of BI CMi is the presence of a number of close frequency pairs in the power spectrum with separations as small as 0.01 cycle d−1.
A rotational velocity of  was determined from a high-dispersion spectrum. From phase differences, the dominant modes can be identified with ℓ values from 0 to 2. The spectral type and evolutionary status of BI CMi are examined. |
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| Keywords: | techniques: photometric stars: individual: BI CMi stars: oscillations stars: rotation δ Scuti |
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