Ages and fundamental properties of<i>Kepler</i>exoplanet host stars from asteroseismology

Aguirre, S.; Davies, G. R.; Basu, Sarbani; Christensen‐Dalsgaard, J.; Creevey, O.; Metcalfe, T. S.; Bedding, Timothy R.; Casagrande, Luca; Handberg, R.; Lund, M. N.; Nissen, P. E.; Chaplin, W. J.; Huber, Daniel; Serenelli, Aldo; Stello, Dennis; Eylen, Vincent Van; Campante, Tiago L.; Elsworth, Y.; Gilliland, Ronald L.; Hekker, S.; Karoff, C.; Kawaler, Steven D.; Kjeldsen, H.; Lundkvist, M.

doi:10.1093/mnras/stv1388

Cited by 341 publications

(359 citation statements)

References 141 publications

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“…Below 20 F ⊕ (where F ⊕ is the flux received by Earth), bulk densities range from 6.3 g cm −3 (rocky) to less than 0.05 g cm −3 . Low-mass planets that have incident fluxes (F) greater than ∼300 times that of Earth are predominantly rocky-in this mass range only Kepler-4 b receives more than 300 F ⊕ and must retain a deep atmosphere, although this case is complicated since the host has likely evolved off the main sequence, increasing the incident flux (Silva Aguirre et al 2015). Hence, the range of planet densities seen in low-mass exoplanets appears strongly anticorrelated with incident flux (Jontof-Hutter et al 2014).…”

Section: 9±54mentioning

confidence: 99%

SECURE MASS MEASUREMENTS FROM TRANSIT TIMING: 10 KEPLER EXOPLANETS BETWEEN 3 AND 8 M _⊕ WITH DIVERSE DENSITIES AND INCIDENT FLUXES

Jontof-Hutter

Ford

Rowe

et al. 2016

ApJ

178

147

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We infer dynamical masses in eight multiplanet systems using transit times measured from Keplerʼs complete dataset, including short-cadence data where available. Of the 18dynamical masses that we infer, 10pass multiple tests for robustness. These are in systemsKepler-26 (KOI-250), Kepler-29 (KOI-738), Kepler-60 (KOI-2086), , and Kepler-307 (KOI-1576). Kepler-105 c has a radius of 1.3 R ⊕ and a density consistent with an Earth-like composition. Strong transit timing variation(TTV) signals were detected from additional planets, but their inferred masses were sensitive to outliers or consistent solutions could not be found with independently measured transit times, including planets orbitingKepler-49 (KOI-248), Kepler-57 (KOI-1270), Kepler-105 (KOI-115), and Kepler-177 (KOI-523). Nonetheless, strong upper limits on the mass of Kepler-177 c imply an extremely low density of∼0.1 g cm −3 . In most cases, individual orbital eccentricities were poorly constrained owingto degeneracies in TTV inversion. For five planet pairs in our sample, strong secular interactions imply a moderatetohigh likelihood of apsidal alignment over a wide range of possible eccentricities. We also find solutions for the three planets known to orbit Kepler-60 in a Laplace-like resonance chain. However, nonlibrating solutions also match the transittiming data. For six systems, we calculate more precise stellar parameters than previously known, enabling useful constraints on planetary densities where we have secure mass measurements. Placing these exoplanets on the mass-radius diagram, we find thata wide range of densities isobserved among sub-Neptune-mass planets and that the range in observed densities is anticorrelated with incident flux.

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Section: 9±54mentioning

confidence: 99%

SECURE MASS MEASUREMENTS FROM TRANSIT TIMING: 10 KEPLER EXOPLANETS BETWEEN 3 AND 8 M _⊕ WITH DIVERSE DENSITIES AND INCIDENT FLUXES

Jontof-Hutter

Ford

Rowe

et al. 2016

ApJ

178

147

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“…With the advent of the Kepler (Borucki et al 2010) and CoRoT (Baglin et al 2006) space missions, time series measuring stellar variability of very-high quality have become widely available. Analysis of these time series can deliver precise estimates of stellar ages Lebreton et al 2014;Meibom et al 2015;Metcalfe et al 2015;Miglio et al 2013b;Silva Aguirre et al 2015) -a quantity critical for reconstructing the history of the Milky Way. With the re-purposed Kepler mission K2 (Howell et al 2014) currently capturing solar-like oscillations Stello et al 2015) in a number of different galactic directions, and the future missions of TESS (Ricker et al 2014) and PLATO (Rauer et al 2014) adding to this, ages for many thousands of stars in many different galactic distances and directions present an exciting possibility.…”

Section: Introductionmentioning

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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“…Similarly, the best-fitting AMP model of HD 176465 B has a comparable mass to the AMP model of HD 176465 A while also having a low initial helium abundance. This degeneracy between mass and helium abundance is well-known in asteroseismic modelling of solar-like oscillations (see Silva Aguirre et al 2015). As discussed, the ASTFIT and BASTA methods have circumvented this problem by enforcing ∆Y/∆Z = 1.4.…”

Section: Modellingmentioning

confidence: 97%

“…The ASTFIT and BASTA methods are both described by Silva Aguirre et al (2015). While both methods use the same input physics (including a solar-calibrated mixing length parameter, α), the ASTFIT method uses models calculated with astec, whereas the BASTA uses models calculated with the Garching Stellar Evolution Code (garstec; Weiss & Schlattl 2008).…”

Section: Modellingmentioning

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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Ages and fundamental properties ofKeplerexoplanet host stars from asteroseismology

Cited by 341 publications

References 141 publications

SECURE MASS MEASUREMENTS FROM TRANSIT TIMING: 10 KEPLER EXOPLANETS BETWEEN 3 AND 8 M _⊕ WITH DIVERSE DENSITIES AND INCIDENT FLUXES

SECURE MASS MEASUREMENTS FROM TRANSIT TIMING: 10 KEPLER EXOPLANETS BETWEEN 3 AND 8 M _⊕ WITH DIVERSE DENSITIES AND INCIDENT FLUXES

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

Keplerobservations of the asteroseismic binary HD 176465

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Ages and fundamental properties ofKeplerexoplanet host stars from asteroseismology

Cited by 341 publications

References 141 publications

SECURE MASS MEASUREMENTS FROM TRANSIT TIMING: 10 KEPLER EXOPLANETS BETWEEN 3 AND 8 M ⊕ WITH DIVERSE DENSITIES AND INCIDENT FLUXES

SECURE MASS MEASUREMENTS FROM TRANSIT TIMING: 10 KEPLER EXOPLANETS BETWEEN 3 AND 8 M ⊕ WITH DIVERSE DENSITIES AND INCIDENT FLUXES

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

Keplerobservations of the asteroseismic binary HD 176465

Contact Info

Product

Resources

About

SECURE MASS MEASUREMENTS FROM TRANSIT TIMING: 10 KEPLER EXOPLANETS BETWEEN 3 AND 8 M _⊕ WITH DIVERSE DENSITIES AND INCIDENT FLUXES

SECURE MASS MEASUREMENTS FROM TRANSIT TIMING: 10 KEPLER EXOPLANETS BETWEEN 3 AND 8 M _⊕ WITH DIVERSE DENSITIES AND INCIDENT FLUXES