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Description
Kepler produces a large amount of data used for asteroseismological analyses, particularly of solar-like stars and red giants. The mode amplitudes observed in the Kepler spectral band have to be converted into bolometric amplitudes to be compared to models. We give a simple bolometric correction for the amplitudes of radial modes observed with Kepler, as well as the relative visibilities of non-radial modes. We numerically compute the bolometric correction c_K-bol_ and mode visibilities, for different effective temperatures Teff within the range 4000-7500K, using a similar approach to a recent one from the literature. We derive a law for the correction to bolometric values: c_K-bol_=1+a_1_(Teff-To)+a_2_(Teff-To)^2^, with To=5934K, a_1_=1.349e-4K^-1^, and a_2_=-3.120e-9K^-2^ or, alternatively, as the power law c_K-bol_=(Teff/To)^alpha^ with alpha=0.80. We give tabulated values for the mode visibilities based on limb-darkening, computed from ATLAS9 model atmospheres for Teff in [4000,7500]K, logg in [2.5,4.5], and [M/H] in [-1.0,+1.0]. We show that using LD profiles already integrated over the spectral band provides quick and good approximations for visibilities. We point out the limits of these classical visibility estimations.
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