SIMBAD references

2018ApJ...857..119B - Astrophys. J., 857, 119-119 (2018/April-3)

Asymmetry of line profiles of stellar oscillations measured by Kepler for ensembles of solar-like oscillators: impact on mode frequencies and dependence on effective temperature.

BENOMAR O., GOUPIL M., BELKACEM K., APPOURCHAUX T., NIELSEN M.B., BAZOT M., GIZON L., HANASOGE S., SREENIVASAN K.R. and MARCHAND B.

Abstract (from CDS):

Oscillation properties are usually measured by fitting symmetric Lorentzian profiles to the power spectra of Sun-like stars. However, the line profiles of solar oscillations have been observed to be asymmetrical for the Sun. The physical origin of this line asymmetry is not fully understood; though, it should depend on the depth dependence of the source of wave excitation (convective turbulence) and details of the observable (velocity or intensity). For oscillations of the Sun, it has been shown that neglecting the asymmetry leads to systematic errors in the frequency determination. This could subsequently affect the results of seismic inferences of the solar internal structure. Using light curves from the Kepler spacecraft, we have measured mode asymmetries in 43 stars. We confirm that neglecting the asymmetry leads to systematic errors that can exceed the 1σ confidence intervals for seismic observations longer than one year. Therefore, the application of an asymmetric Lorentzian profile should be favored to improve the accuracy of the internal stellar structure and stellar fundamental parameters. We also show that the asymmetry changes sign between cool Sun-like stars and hotter stars. This provides the best constraints to date on the location of the excitation sources across the Hertzsprung-Russel diagram.

Abstract Copyright: © 2018. The American Astronomical Society. All rights reserved.

Journal keyword(s): methods: data analysis - stars: interiors - stars: oscillations including pulsations

VizieR on-line data: <Available at CDS (J/ApJ/857/119): stars.dat table1.dat>

Simbad objects: 43

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2019.10.21-13:28:46

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