Prospects for asteroseismology

Christensen‐Dalsgaard, J.; Houdek, G.

doi:10.1007/s10509-009-0227-z

Cited by 59 publications

(51 citation statements)

References 96 publications

(90 reference statements)

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“…As seen, only a few stars, including the Sun, actually adhere to the expectation from the asymptotic relation. This was similarly found by Christensen-Dalsgaard & Houdek (2010) 7 for α Cen A (Bedding et al 2004), while α Cen B (Kjeldsen et al 2005) was found to fulfill the asymptotic relation. As explained by Christensen-Dalsgaard & Houdek (2010) this reflects a rapid variation of the sound speed in the core of α Cen A from its more evolved state due to its higher mass compared to the B component.…”

Section: Average Seismic Parameterssupporting

confidence: 72%

“…This was similarly found by Christensen-Dalsgaard & Houdek (2010) 7 for α Cen A (Bedding et al 2004), while α Cen B (Kjeldsen et al 2005) was found to fulfill the asymptotic relation. As explained by Christensen-Dalsgaard & Houdek (2010) this reflects a rapid variation of the sound speed in the core of α Cen A from its more evolved state due to its higher mass compared to the B component. Similarly, Verma et al (2014) found an increasing departure from the asymptotic description of the oscillation frequencies while fitting the signatures of the acoustic glitches.…”

Section: Average Seismic Parameterssupporting

confidence: 72%

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Standing on the Shoulders of Dwarfs: the Kepler Asteroseismic LEGACY Sample. I. Oscillation Mode Parameters

Lund

Aguirre

Davies

et al. 2017

ApJ

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227

223

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The advent of space-based missions like Kepler has revolutionized the study of solar-type stars, particularly through the measurement and modeling of their resonant modes of oscillation. Here we analyze a sample of 66 Kepler main-sequence stars showing solar-like oscillations as part of the Kepler seismic LEGACY project. We use Kepler short-cadence data, of which each star has at least 12 months, to create frequency power spectra optimized for asteroseismology. For each star we identify its modes of oscillation and extract parameters such as frequency, amplitude, and line width using a Bayesian Markov chain Monte Carlo 'peak-bagging' approach. We report the extracted mode parameters for all 66 stars, as well as derived quantities such as frequency difference ratios, the large and small separations ∆ν and δν 02 ; the behavior of line widths with frequency and line widths at ν max with T eff , for which we derive parametrizations; and behavior of mode visibilities. These average properties can be applied in future peak-bagging exercises to better constrain the parameters of the stellar oscillation spectra. The frequencies and frequency ratios can tightly constrain the fundamental parameters of these solar-type stars, and mode line widths and amplitudes can test models of mode damping and excitation.

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Section: Average Seismic Parameterssupporting

confidence: 72%

Section: Average Seismic Parameterssupporting

confidence: 72%

Standing on the Shoulders of Dwarfs: the Kepler Asteroseismic LEGACY Sample. I. Oscillation Mode Parameters

Lund

Aguirre

Davies

et al. 2017

ApJ

Self Cite

227

223

View full text Add to dashboard Cite

show abstract

“…In this respect, asteroseismology is thought to be the most powerful tool for studying the inner properties of stars through the observation of stellar oscillations (e.g. Aerts et al 2008;Christensen-Dalsgaard & Houdek 2010, and references therein).…”

Section: Effects Of Mixing In Semiconvective Layersmentioning

confidence: 99%

Constraining mixing processes in stellar cores using asteroseismology

Aguirre

Ballot

Serenelli

et al. 2011

A&A

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Context. The overall evolution of low-mass stars is heavily influenced by the processes occurring in the stellar interior. In particular, mixing processes in convectively unstable zones and overshooting regions affect the resulting observables and main sequence lifetime. Aims. We aim to study the effects of different convective boundary definitions and mixing prescriptions in convective cores of lowmass stars and to distinguish the existence, size, and evolutionary stage of the central mixed zone by means of asteroseismology. Methods. We implemented the Ledoux criterion for convection in our stellar evolution code, together with a time-dependent diffusive approach for mixing of elements when semiconvective zones are present. We compared models with masses ranging from 1.1 M to 2 M computed with two different criteria for convective boundary definition and included different mixing prescriptions within and beyond the formal limits of the convective regions. Using calculations of adiabatic oscillations frequencies for a large set of models, we developed an asteroseismic diagnosis using only l = 0 and l = 1 modes based on the ratios of small to large separations r 01 and r 10 defined by Roxburgh & Vorontsov (2003, A&A, 411, 215). We analyzed the sensitivity of this seismic tool to the central conditions of the star during the main sequence evolution. Results. The seismic variables r 01 and r 10 are almost linear in the expected observable frequency range, and we show that their slope depends simultaneously on the central hydrogen content, the extent of the convective core, and the amplitude of the sound-speed discontinuity at the core boundary. By considering about 25 modes and an accuracy in the frequency determinations as expected from the CoRoT and Kepler missions, the technique we propose allows us to detect the presence of a convective core and to discriminate the different sizes of the homogeneously mixed central region without the need for a strong prior knowledge on the stellar mass.

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“…[26] determined the profile of opacity enhancements that would make a solar model with AGSS09 abundances have the same structure as Model S by [27]. This standard solar model was evolved with the classic GN93 abundances (dashed, black curve in Fig.…”

Section: Opacity Solutions To the Solar Abundance Problemmentioning

confidence: 99%

An opaque Sun? The potential for future, higher opacities to solve the solar abundance problem

Trampedach

2017

EPJ Web Conf.

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Abstract. Last year Bailey et al. announced their measurement of iron opacity that increases the Rosseland mean at the base of the solar convection zone by 7%. I ask what happens if the absorption by other elements is also stronger than predicted so far. Artificially increasing the absorption by other elements, proportional to the number of bound electrons in the absorber (reflecting our remaining ignorance of atomic physics) gives an opacity increase for a solar model, that has the potential to solve the long-standing solar abundance problem. Conclusion: Opacities are the likely source of the solar abundance problem, and the solar abundances are likely closer to those of than to the various classic sets of abundances.

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Prospects for asteroseismology

Cited by 59 publications

References 96 publications

Standing on the Shoulders of Dwarfs: the Kepler Asteroseismic LEGACY Sample. I. Oscillation Mode Parameters

Standing on the Shoulders of Dwarfs: the Kepler Asteroseismic LEGACY Sample. I. Oscillation Mode Parameters

Constraining mixing processes in stellar cores using asteroseismology

An opaque Sun? The potential for future, higher opacities to solve the solar abundance problem

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