Open Access29 frequencies for the δ Scuti variable BI CMi: the 1997–2000 multisite campaigns
Author(s) -
Breger M.,
Garrido R.,
Handler G.,
Wood M.A.,
Shobbrook R.R.,
Bischof K.M.,
Rodler F.,
Gray R. O.,
Stankov A.,
Martinez P.,
O'Donoghue D.,
Szabó R.,
Zima W.,
Kaye A. B.,
Barban C.,
Heiter U.
Publication year - 2002
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1046/j.1365-8711.2002.04970.x
Subject(s) - physics , instability strip , photometry (optics) , astrophysics , instability , spectral density , spectral line , low frequency , stars , astronomy , cepheid variable , statistics , mathematics , mechanics
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.