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J/A+A/531/A124      Visibilities 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.124B
ADC_Keywords: Models, atmosphere Keywords: asteroseismology - stars: atmospheres - stars: solar-type Abstract: 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 cK-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: cK-bol=1+a1(Teff-To)+a2(Teff-To)2, with To=5934K, a1=1.349e-4K-1, and a2=-3.120e-9K-2 or, alternatively, as the power law cK-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): Vl 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, V0=1. Here the values of Vl2 are tabulated, they correspond to mode visibilities in oscillation power spectra. The total visibility Vt2 is defined as the sum of Vl2 l=0 to infinity.
Acknowledgements: Jerome Ballot, jballot(at)ast.obs-mip.fr
(End) Jerome Ballot [IRAP, France], Patricia Vannier [CDS] 07-Jun-2011
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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