J/A+A/531/A124Visibilities of stellar oscillation modes (Ballot+, 2011)

Visibilities and bolometric corrections for stellar oscillation modes observed by Kepler. Ballot J., Barban C., van't Veer-Menneret C. <Astron. Astrophys. 531, A124 (2011)> =2011A&A...531A.124BADC_Keywords: Models, atmosphereKeywords: asteroseismology - stars: atmospheres - stars: solar-typeAbstract: 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.Description: These are computations of visibilities of non-radial modes for the Kepler mission.File Summary:

FileName Lrecl Records Explanations

ReadMe 80 . This file table1.dat 34 487 Visibilities of oscillation modes for Kepler

See also: J/A+A/529/A89 : Kepler satellite variability study (Debosscher+, 2011)Byte-by-byte Description of file: table1.dat

Bytes Format Units Label Explanations

1- 4 I4 K Teff [4000,7500] Stellar effective temperature 6- 8 F3.1 [cm/s+2] logg [2.5,4.5] Stellar surface gravity 10- 13 F4.1 [Sun] M/H [-1.0,+1.0] Stellar metallicity (1) 15- 18 F4.2 --- V2.t Total visibilities (2) 20- 23 F4.2 --- V2.1 Visibilities for l=1 mode (2) 25- 28 F4.2 --- V2.2 Visibilities for l=2 mode (2) 30- 34 F5.3 --- V2.3 Visibilities for l=3 mode (2)

Note (1): The metallicity is log[metal/H]-log[(metal/H)_☉].Note (2): V_{l}is the visibility of a mode of degree l, i.e. the apparent amplitude of this mode compared to a radial mode (l=0) that would have the same intrinsic amplitude at the surface of the star. By definition, V_{0}=1. Here the values of V_{l}^{2}are tabulated, they correspond to mode visibilities in oscillation power spectra. The total visibility V_{t}^{2}is defined as the sum of V_{l}^{2}l=0 to infinity.

Acknowledgements: Jerome Ballot, jballot(at)ast.obs-mip.fr(End)Jerome Ballot [IRAP, France], Patricia Vannier [CDS] 07-Jun-2011

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