ASTEROSEISMOLOGY OF EVOLVED STARS WITH
                    <i>KEPLER</i>
                    : A NEW WAY TO CONSTRAIN STELLAR INTERIORS USING MODE INERTIAS

Benomar, O.; Belkacem, K.; Bedding, Timothy R.; Stello, Dennis; Mauro, M. P. Di; Ventura, R.; Mosser, B.; Goupil, M. J.; Samadi, R.; García, Rafael A.

doi:10.1088/2041-8205/781/2/l29

Cited by 61 publications

(66 citation statements)

References 41 publications

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“…Recently, Benomar et al (2014) remarked that the ratio I 1 /I 0 of the inertia of dipole modes compared to radial modes may provide an alternative to using mixed-mode frequencies and give essentially the same information as the mixed-mode asymptotic equation. We confirm that this is the case: their function I 1 /I 0 can be related to ζ if we assume that the difference between the total inertia of mixed modes and the contribution of the radiative cavity only exactly corresponds to the inertia of radial modes.…”

Section: Comparison With Previous Workmentioning

confidence: 99%

Period spacings in red giants

Mosser

Vrard

Belkacem

et al. 2015

A&A

Self Cite

104

222

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Context. Asteroseismology allows us to probe the physical conditions inside the core of red giant stars. This process relies on the properties of the global oscillations with a mixed character that are highly sensitive to the physical properties of the core. However, overlapping rotational splittings and mixed-mode spacings result in complex structures in the mixed-mode pattern, which severely complicates its identification and the measurement of the asymptotic period spacing. Aims. This work aims at disentangling the rotational splittings from the mixed-mode spacings in order to open the way to a fully automated analysis of large data sets.Methods. An analytical development of the mixed-mode asymptotic expansion is used to derive the period spacing between two consecutive mixed modes. The échelle diagrams constructed with the appropriately stretched periods are used to exhibit the structure of the gravity modes and of the rotational splittings. Results. We propose a new view of the mixed-mode oscillation pattern based on corrected periods, called stretched periods, that mimic the evenly spaced gravity-mode pattern. This provides a direct understanding of all oscillation components, even in the case of rapid rotation. In this way, the measurement of the asymptotic period spacing and the signature of the structural glitches on mixed modes can be performed easily. Conclusions. This work makes it possible to derive all seismic global parameters in an automated way, including the identification of the different rotational multiplets and the measurement of the rotational splitting, even when this splitting is significantly larger than the period spacing. Revealing buoyancy glitches provides a detailed view of the radiative core.

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Section: Comparison With Previous Workmentioning

confidence: 99%

Period spacings in red giants

Mosser

Vrard

Belkacem

et al. 2015

A&A

Self Cite

104

222

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“…From Benomar et al (2014), we state that the ratio of the inertia of a radial and dipole mode can be approximated using…”

Section: Detailed Modelling Of the Power Spectrummentioning

confidence: 99%

Asteroseismology of red giants: From analysing light curves to estimating ages

Davies

Miglio

2016

Astron Nachr

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Asteroseismology has started to provide constraints on stellar properties that will be essential to accurately reconstruct the history of the Milky Way. Here we look at the information content in data sets representing current and future space missions (CoRoT, Kepler, K2, TESS, and PLATO) for red giant stars. We describe techniques for extracting the information in the frequency power spectrum and apply these techniques to Kepler data sets of different observing length to represent the different space missions. We demonstrate that for KIC 12008916, a low-luminosity red giant branch star, we can extract useful information from all data sets, and for all but the shortest data set we obtain good constraint on the g-mode period spacing and core rotation rates. We discuss how the high precision in these parameters will constrain the stellar properties of stellar radius, distance, mass and age. We show that high precision can be achieved in mass and hence age when values of the g-mode period spacing are available. We caution that tests to establish the accuracy of asteroseismic masses and ages are still "work in progress".

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“…Beck et al 2011;Bedding et al 2011;Mosser et al 2011;Stello et al 2013;Benomar et al 2013Benomar et al , 2014 -including some belonging to a few clusters Basu et al 2011) -it is now possible to infer the core rotation rate of these stars (Beck et al 2012;Mosser et al 2012;Di Mauro et al 2013;Goupil et al 2013), which is still difficult to determine for solar-like stars and even for the Sun (e.g. García et al 2004García et al , 2007García et al , 2008a.…”

Section: Introductionmentioning

confidence: 99%

Rotation and magnetism ofKeplerpulsating solar-like stars

García

Ceillier

Salabert

et al. 2014

A&A

262

344

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Kepler ultra-high precision photometry of long and continuous observations provides a unique dataset in which surface rotation and variability can be studied for thousands of stars. Because many of these old field stars also have independently measured asteroseismic ages, measurements of rotation and activity are particularly interesting in the context of age-rotation-activity relations. In particular, age-rotation relations generally lack good calibrators at old ages, a problem that this Kepler sample of old-field stars is uniquely suited to address. We study the surface rotation and photometric magnetic activity of a subset of 540 solar-like stars on the mainsequence and the subgiant branch for which stellar pulsations have been measured. The rotation period was determined by comparing the results from two different analysis methods: i) the projection onto the frequency domain of the time-period analysis, and ii) the autocorrelation function of the light curves. Reliable surface rotation rates were then extracted by comparing the results from two different sets of calibrated data and from the two complementary analyses. General photometric levels of magnetic activity in this sample of stars were also extracted by using a photometric activity index, which takes into account the rotation period of the stars. We report rotation periods for 310 out of 540 targets (excluding known binaries and candidate planet-host stars); our measurements span a range of 1 to 100 days. The photometric magnetic activity levels of these stars were computed, and for 61.5% of the dwarfs, this level is similar to the range, from minimum to maximum, of the solar magnetic activity. We demonstrate that hot dwarfs, cool dwarfs, and subgiants have very different rotation-age relationships, highlighting the importance of separating out distinct populations when interpreting stellar rotation periods. Our sample of cool dwarf stars with age and metallicity data of the highest quality is consistent with gyrochronology relations reported in the literature.

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ASTEROSEISMOLOGY OF EVOLVED STARS WITH KEPLER : A NEW WAY TO CONSTRAIN STELLAR INTERIORS USING MODE INERTIAS

Cited by 61 publications

References 41 publications

Period spacings in red giants

Period spacings in red giants

Asteroseismology of red giants: From analysing light curves to estimating ages

Rotation and magnetism ofKeplerpulsating solar-like stars

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