The ratio of small to large separations of acoustic oscillations as a diagnostic of the interior of solar-like stars

Roxburgh, I. W.; Vorontsov, S. V.

doi:10.1051/0004-6361:20031318

Cited by 307 publications

(359 citation statements)

References 11 publications

Supporting

Mentioning

355

Contrasting

Order By: Relevance

“…On the other hand Creevey and to some extent Verma are less sensitive to the surface frequency correction because of the use of frequency separations and ratios. For these latter, the lack of sensitivity was explained by Roxburgh & Vorontsov (2003b). The additional regularisation parameters of Verma may also contribute to a different χ 2 .…”

Section: Analysis Of Model Differencesmentioning

confidence: 99%

A seismic and gravitationally bound double star observed byKepler

Appourchaux

Antia

Ball

et al. 2015

A&A

View full text Add to dashboard Cite

Context. Solar-like oscillations have been observed by Kepler and CoRoT in many solar-type stars, thereby providing a way to probe stars using asteroseismology. Aims. The derivation of stellar parameters has usually been done with single stars. The aim of the paper is to derive the stellar parameters of a double-star system (HIP 93511), for which an interferometric orbit has been observed along with asteroseismic measurements. Methods. We used a time series of nearly two years of data for the double star to detect the two oscillation-mode envelopes that appear in the power spectrum. Using a new scaling relation based on luminosity, we derived the radius and mass of each star. We derived the age of each star using two proxies: one based upon the large frequency separation and a new one based upon the small frequency separation. Using stellar modelling, the mode frequencies allowed us to derive the radius, the mass, and the age of each component. In addition, speckle interferometry performed since 2006 has enabled us to recover the orbit of the system and the total mass of the system. Results. From the determination of the orbit, the total mass of the system is 2.34 +0.45 −0.33 M . The total seismic mass using scaling relations is 2.47 ± 0.07 M . The seismic age derived using the new proxy based upon the small frequency separation is 3.5 ± 0.3 Gyr. Based on stellar modelling, the mean common age of the system is 2.7-3.9 Gyr. The mean total seismic mass of the system is 2.34-2.53 M consistent with what we determined independently with the orbit. The stellar models provide the mean radius, mass, and age of the stars as R A = 1.82−1.87 R , M A = 1.25−1.39 M , Age A = 2.6-3.5 Gyr; R B = 1.22−1.25 R , M B = 1.08−1.14 M , Age B = 3.35-4.21 Gyr. The models provide two sets of values for Star A: [1.25-1.27] M and [1.34-1.39] M . We detect a convective core in Star A, while Star B does not have any. For the metallicity of the binary system of Z ≈ 0.02, we set the limit between stars having a convective core in the range [1.14-1.25] M .

show abstract

Section: Analysis Of Model Differencesmentioning

confidence: 99%

A seismic and gravitationally bound double star observed byKepler

Appourchaux

Antia

Ball

et al. 2015

A&A

View full text Add to dashboard Cite

show abstract

“…In these cases, instead of fitting for the global asteroseismic parameters the Bayesian schemes aim at reproducing either the individual frequencies of oscillations or combinations of them. The first approach usually relies on an empirical surface correction to account for incomplete modelling of the outer stellar layers in 1-D hydrostatic codes (e.g., Kjeldsen et al 2008), while the latter suppresses the influence of these layers by building frequency rations (Roxburgh & Vorontsov 2003). Recently Lebreton & Goupil (2014) showed that the most precise asterosesimic ages for dwarfs are those obtained using the frequency ratios as fitting observables as they are sensitive to the innermost layers of the star.…”

Section: Improvements For Dwarfs and Subgiants: Individual Frequenciesmentioning

confidence: 99%

Asteroseismic age determination for dwarfs and giants

Aguirre

Serenelli

2016

Astron Nachr

View full text Add to dashboard Cite

Asteroseismology can make a substantial contribution to our understanding of the formation history and evolution of our Galaxy by providing precisely determined stellar properties for thousands of stars in different regions of the Milky Way. We present here the different sets of observables used in determining asteroseismic stellar properties, the typical level of precision obtained, the current status of results for ages of dwarfs and giants and the improvements than can be expected in the near future in the context of Galactic archaeology.

show abstract

“…Roxburgh & Vorontsov (2003) have demonstrated that the ratio of the small to large separations of acoustic oscillations is essentially independent of the structure of the outer layers. We thus renormalize the small spacings by considering the ratios δν 02 (n)/∆ν(n, ℓ = 1), δν 13 (n)/∆ν(n + 1, ℓ = 0) and δν 01 (n)/∆ν(n, ℓ = 1) where the large separation is given by:…”

Section: Fig 4 Relative Frequency Differences Between the Gravity Mmentioning

confidence: 99%

Sensitivity of the sub-photospheric flow fields inferred from ring-diagram analysis to the change on the solar model

Zaatri

Provost

Corbard

et al. 2009

Astrophys Space Sci

View full text Add to dashboard Cite

Context. The most recent determination of the solar chemical composition, using a time-dependent, 3D hydrodynamical model of the solar atmosphere, exhibits a significant decrease of C, N, O abundances compared to their previous values. Solar models that use these new abundances are not consistent with helioseismological determinations of the sound speed profile, the surface helium abundance and the convection zone depth. Aims. We investigate the effect of changes of solar abundances on low degree p-mode and g-mode characteristics which are strong constraints of the solar core. We consider particularly the increase of neon abundance in the new solar mixture in order to reduce the discrepancy between models using new abundances and helioseismology. Methods. The observational determinations of solar frequencies from the GOLF instrument are used to test solar models computed with different chemical compositions. We consider in particular the normalized small frequency spacings in the low degree p-mode frequency range. Results. Low-degree small frequency spacings are very sensitive to changes in the heavy-element abundances, notably neon. We show that by considering all the seismic constraints, including the small frequency spacings, a rather large increase of neon abundance by about (0.5 ± 0.05)dex can be a good solution to the discrepancy between solar models that use new abundances and low degree helioseismology, subject to adjusting slightly the solar age and the highest abundances. We also show that the change in solar abundances, notably neon, considerably affects g-mode frequencies, with relative frequency differences between the old and the new models higher than 1.5%.

show abstract

The ratio of small to large separations of acoustic oscillations as a diagnostic of the interior of solar-like stars

Cited by 307 publications

References 11 publications

A seismic and gravitationally bound double star observed byKepler

A seismic and gravitationally bound double star observed byKepler

Asteroseismic age determination for dwarfs and giants

Sensitivity of the sub-photospheric flow fields inferred from ring-diagram analysis to the change on the solar model

Contact Info

Product

Resources

About