Surface Activity and Oscillation Amplitudes of Red Giants in Eclipsing Binaries

Gaulme, P.; Jackiewicz, Jason; Appourchaux, T.; Mosser, B.

doi:10.1088/0004-637x/785/1/5

Cited by 85 publications

(151 citation statements)

References 30 publications

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“…The methods we use are described in Gaulme et al (2013Gaulme et al ( , 2014, and here we provide a summary. The way light curves are processed is of prime importance becausepart of the conclusions of this paper depends on our ability to provide reliable estimates of stellar radii.…”

Section: Kepler Photometric Light Curvesmentioning

confidence: 99%

Testing the Asteroseismic Scaling Relations for Red Giants With Eclipsing Binaries Observed by Kepler

Gaulme

McKeever

Jackiewicz

et al. 2016

ApJ

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175

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Given the potential of ensemble asteroseismology for understanding fundamental properties of large numbers of stars, it is critical to determine the accuracy of the scaling relations on which these measurements are based. From several powerful validation techniques, all indications so far show that stellar radius estimates from the asteroseismic scaling relations are accurate to within a few percent. Eclipsing binary systems hosting at least one star with detectable solar-like oscillations constitute the ideal test objects for validating asteroseismic radius and mass inferences. By combining radial velocity (RV) measurements and photometric time series of eclipses, it is possible to determine the masses and radii of each component of a double-lined spectroscopic binary. We report the results of a four-year RV survey performed with the échelle spectrometer of the Astrophysical Research Consortium's 3.5 m telescope and the APOGEE spectrometer at Apache Point Observatory. We compare the masses and radii of 10 red giants (RGs) obtained by combining radial velocities and eclipse photometry with the estimates from the asteroseismic scaling relations. We find that the asteroseismic scaling relations overestimate RG radii by about 5% on average and masses by about 15% for stars at various stages of RG evolution. Systematic overestimation of mass leads to underestimation of stellar age, which can have important implications for ensemble asteroseismology used for Galactic studies. As part of a second objective, where asteroseismology is used for understanding binary systems, we confirm that oscillations of RGs in close binaries can be suppressed enough to be undetectable, ahypothesis that was proposed in a previous work.

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Section: Kepler Photometric Light Curvesmentioning

confidence: 99%

Testing the Asteroseismic Scaling Relations for Red Giants With Eclipsing Binaries Observed by Kepler

Gaulme

McKeever

Jackiewicz

et al. 2016

ApJ

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175

307

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“…Among dwarfs, comparing asteroseismic radii to radii from Hipparcos parallax and bolometric flux (Silva Aguirre et al 2012) and to radii from interferometry (Huber et al 2012) show agreement to within 5%. RGB radii comparisons show mixed results (see Huber et al 2012;Frandsen et al 2013;Gaulme et al 2014;Brogaard et al 2016;Gaulme et al 2016).…”

Section: Tgas-asteroseismic Parallax Zeropointmentioning

confidence: 99%

Evidence for Spatially Correlated Gaia Parallax Errors in the Kepler Field

Zinn

Huber

Pinsonneault

et al. 2017

ApJ

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We present evidence for a spatially-dependent systematic error in the first data release of Gaia parallaxes based on comparisons to asteroseismic parallaxes in the Kepler field, and present a parametrized model of the angular dependence of these systematics. We report an error of 0.059−0.004 mas on scales of 0.3deg, which decreases for larger scales to become 0.011−0.004 mas at 8deg. This is consistent with the ∼ 2% zeropoint offset for the whole sample discussed by Huber et al., and is compatible with the effect predicted by the Gaia team. Our results are robust to dust prescriptions and choices in temperature scales used to calculate asteroseismic parallaxes. We also do not find evidence for significant differences in the signal when using red clump versus red giant stars. Our approach allows us to quantify and map the correlations in an astrophysically interesting field, resulting in a parametrized model of the spatial systematics that can be used to construct a covariance matrix for any work that relies upon TGAS parallaxes.

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“…Despite these challenges, such systems will provide further tests of stellar structure and evolution when they are found, just as systems with a single oscillating red giant have already (e.g. Hekker et al 2010b;Frandsen et al 2013;Gaulme et al 2013Gaulme et al , 2014Beck et al 2014;Rawls et al 2016). With the future missions TESS (Ricker et al 2015;Campante et al 2016) and PLATO (Rauer et al 2014) to provide asteroseismic data for many more systems, there will be good opportunities to find more such asteroseismic binary systems.…”

Section: Discussionmentioning

confidence: 99%

“…Mathur et al 2013), particularly amongst the many red giants that have been observed (e.g. Hekker et al 2010b;Frandsen et al 2013;Gaulme et al 2013Gaulme et al , 2014Beck et al 2014;Rawls et al 2016). In addition, KIC 4471379 (Murphy et al 2014) is a binary in which both components are δ Scuti pulsators, while KIC 10080943 (Schmid et al 2015;Keen et al 2015) has two γ Doradus/δ Scuti hybrids.…”

Section: Introductionmentioning

confidence: 99%

Keplerobservations of the asteroseismic binary HD 176465

White

Benomar

Aguirre

et al. 2017

A&A

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Binary star systems are important for understanding stellar structure and evolution, and are especially useful when oscillations can be detected and analysed with asteroseismology. However, only four systems are known in which solar-like oscillations are detected in both components. Here, we analyse the fifth such system, HD 176465, which was observed by Kepler. We carefully analysed the system's power spectrum to measure individual mode frequencies, adapting our methods where necessary to accommodate the fact that both stars oscillate in a similar frequency range. We also modelled the two stars independently by fitting stellar models to the frequencies and complementary parameters. We are able to cleanly separate the oscillation modes in both systems. The stellar models produce compatible ages and initial compositions for the stars, as is expected from their common and contemporaneous origin. Combining the individual ages, the system is about 3.0 ± 0.5 Gyr old. The two components of HD 176465 are young physicallysimilar oscillating solar analogues, the first such system to be found, and provide important constraints for stellar evolution and asteroseismology.

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Surface Activity and Oscillation Amplitudes of Red Giants in Eclipsing Binaries

Cited by 85 publications

References 30 publications

Testing the Asteroseismic Scaling Relations for Red Giants With Eclipsing Binaries Observed by Kepler

Testing the Asteroseismic Scaling Relations for Red Giants With Eclipsing Binaries Observed by Kepler

Evidence for Spatially Correlated Gaia Parallax Errors in the Kepler Field

Keplerobservations of the asteroseismic binary HD 176465

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