Asteroseismology and interferometry

Cunha, M. S.; Aerts, C.; Christensen‐Dalsgaard, J.; Baglin, A.; Bigot, Lionel; Brown, Timothy M.; Catala, C.; Creevey, O.; Souza, A. Domiciano de; Eggenberger, P.; Garcia, Paulo J. V.; Grundahl, F.; Kervella, P.; Kurtz, D. W.; Mathias, P.; Miglio, A.; Monteiro, M. J. P. F. G.; Perrin, G.; Pijpers, F. P.; Pourbaix, D.; Quirrenbach, A.; Rousselet-Perraut, K.; Teixeira, T. C.; Thévenin, F.; Thompson, M. J.

doi:10.1007/s00159-007-0007-0

Cited by 117 publications

(57 citation statements)

References 428 publications

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“…Principle Solar-like oscillations are predominantly acoustic global standing waves. Commonly called p modes, owing to the fact that pressure plays the role of the restoring force, these modes are intrinsically damped and stochastically excited by nearsurface convection (for a review see, e.g., ChristensenDalsgaard 2004;Cunha et al 2007;Chaplin & Miglio 2013). The oscillation modes are characterized by the radial order n, the spherical degree l, and the azimuthal order m. Radial modes have l = 0, whereas non-radial modes have l>0.…”

Section: Estimation Of the Stellar Inclination Anglementioning

confidence: 99%

Spin–orbit Alignment of Exoplanet Systems: Ensemble Analysis Using Asteroseismology

Campante

Lund

Kuszlewicz

et al. 2016

ApJ

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103

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The angle ψ between a planet's orbital axis and the spin axis of its parent star is an important diagnostic of planet formation, migration, and tidal evolution. We seek empirical constraints on ψ by measuring the stellar inclination i s via asteroseismology for an ensemble of 25 solar-type hosts observed with NASA's Kepler satellite. Our results for i s are consistent with alignment at the 2σ level for all stars in the sample, meaning that the system surrounding the red-giant star Kepler-56 remains as the only unambiguous misaligned multiple-planet system detected to date. The availability of a measurement of the projected spin-orbit angle λ for two of the systems allows us to estimate ψ. We find that the orbit of the hot Jupiter HAT-P-7b is likely to be retrograde ( 116 . 4 14.730.2, whereas that of Kepler-25c seems to be well aligned with the stellar spin axis ( 12 . 6 11.0 6.7While the latter result is in apparent contradiction with a statement made previously in the literature that the multi-transiting system Kepler-25 is misaligned, we show that the results are consistent, given the large associated uncertainties. Finally, we perform a hierarchical Bayesian analysis based on the asteroseismic sample in order to recover the underlying distribution of ψ. The ensemble analysis suggests that the directions of the stellar spin and planetary orbital axes are correlated, as conveyed by a tendency of the host stars to display large values of inclination.

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Section: Estimation Of the Stellar Inclination Anglementioning

confidence: 99%

Spin–orbit Alignment of Exoplanet Systems: Ensemble Analysis Using Asteroseismology

Campante

Lund

Kuszlewicz

et al. 2016

ApJ

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103

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“…While the potential of combining asteroseismology and interferometry has been long recognized (see, e.g., Cunha et al 2007), observational constraints have so far restricted an application for cool stars to relatively few bright objects (North et al 2007;Bruntt et al 2010;Bazot et al 2011). Recent technological advances, however, have changed this picture.…”

Section: Introductionmentioning

confidence: 99%

FUNDAMENTAL PROPERTIES OF STARS USING ASTEROSEISMOLOGY FROMKEPLERANDCoRoTAND INTERFEROMETRY FROM THE CHARA ARRAY

Huber

Ireland

Bedding

et al. 2012

ApJ

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221

167

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We present results of a long-baseline interferometry campaign using the PAVO beam combiner at the CHARA Array to measure the angular sizes of five main-sequence stars, one subgiant and four red giant stars for which solarlike oscillations have been detected by either Kepler or CoRoT. By combining interferometric angular diameters, Hipparcos parallaxes, asteroseismic densities, bolometric fluxes, and high-resolution spectroscopy, we derive a full set of near-model-independent fundamental properties for the sample. We first use these properties to test asteroseismic scaling relations for the frequency of maximum power (ν max ) and the large frequency separation (Δν). We find excellent agreement within the observational uncertainties, and empirically show that simple estimates of asteroseismic radii for main-sequence stars are accurate to 4%. We furthermore find good agreement of our measured effective temperatures with spectroscopic and photometric estimates with mean deviations for stars between T eff = 4600-6200 K of −22 ± 32 K (with a scatter of 97 K) and −58 ± 31 K (with a scatter of 93 K), respectively. Finally, we present a first comparison with evolutionary models, and find differences between observed and theoretical properties for the metal-rich main-sequence star HD 173701. We conclude that the constraints presented in this study will have strong potential for testing stellar model physics, in particular when combined with detailed modeling of individual oscillation frequencies.

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“…The success of asteroseismic studies has been shown to depend crucially on the availability of first estimates of basic stellar parameters, such as the effective temperature (T eff ), surface gravity ( g log ), metallicity ( M H [ ]), and projected stellar equatorial rotation velocity (v i sin ; Michel 2006;Cunha et al 2007). These parameters cannot always be directly derived from the Kepler data, as in the case of data with multicolor photometry or spectroscopy.…”

Section: Introductionmentioning

confidence: 99%

LAMOST OBSERVATIONS IN THE KEPLER FIELD. I. DATABASE OF LOW-RESOLUTION SPECTRA

Cat

Ren

et al. 2015

ApJS

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138

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The nearly continuous light curves with micromagnitude precision provided by the space mission Kepler are revolutionizing our view of pulsating stars. They have revealed a vast sea of low-amplitude pulsation modes that were undetectable from Earth. The long time base of Kepler light curves allows for the accurate determination of the frequencies and amplitudes of pulsation modes needed for in-depth asteroseismic modeling. However, for an asteroseismic study to be successful, the first estimates of stellar parameters need to be known and they cannot be derived from the Kepler photometry itself. The Kepler Input Catalog provides values for the effective temperature, surface gravity, and metallicity, but not always with sufficient accuracy. Moreover, information on the chemical composition and rotation rate is lacking. We are collecting low-resolution spectra for objects in the Kepler field of view with the Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST, Xinglong observatory, China). All of the requested fields have now been observed at least once. In this paper, we describe those observations and provide a useful database for the whole astronomical community.

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Asteroseismology and interferometry

Abstract: Astronomy and Astrophysics Review, 14, pp. 217-360, http://dx.doi.org./10.1007/s00159-007-0007-0International audienc

Cited by 117 publications

References 428 publications

Spin–orbit Alignment of Exoplanet Systems: Ensemble Analysis Using Asteroseismology

Spin–orbit Alignment of Exoplanet Systems: Ensemble Analysis Using Asteroseismology

FUNDAMENTAL PROPERTIES OF STARS USING ASTEROSEISMOLOGY FROMKEPLERANDCoRoTAND INTERFEROMETRY FROM THE CHARA ARRAY

LAMOST OBSERVATIONS IN THE KEPLER FIELD. I. DATABASE OF LOW-RESOLUTION SPECTRA

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