Testing stellar evolution models with detached eclipsing binaries

Higl, J.; Weiß, Achim

doi:10.1051/0004-6361/201731008

Cited by 59 publications

(57 citation statements)

References 112 publications

(135 reference statements)

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“…Precise modelling of detached double-lined eclipsing binaries also requires CBM in order to match the observed stellar parameters at concurrent ages Deheuvels et al 2016;Higl & Weiss 2017;Claret & Torres 2018;Constantino & Baraffe 2018;Claret & Torres 2019). Given their ability to break some of the degeneracies in the modelling, these systems offer perhaps our best constraints of main-sequence core overshoot.…”

Section: Modification Of the Composition Profile Through Cbmmentioning

confidence: 99%

Convective boundary mixing in low- and intermediate-mass stars – I. Core properties from pressure-mode asteroseismology

Angelou

Bellinger

Hekker

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Convective boundary mixing (CBM) is ubiquitous in stellar evolution. It is a necessary ingredient in the models in order to match observational constraints from clusters, binaries and single stars alike. We compute 'effective overshoot' measures that reflect the extent of mixing and which can differ significantly from the input overshoot values set in the stellar evolution codes. We use constraints from pressure modes to infer the CBM properties of Kepler and CoRoT main-sequence and subgiant oscillators, as well as in two radial velocity targets (Procyon A and α Cen A). Collectively these targets allow us to identify how measurement precision, stellar spectral type, and overshoot implementation impact the asteroseismic solution. With these new measures we find that the 'effective overshoot' for most stars is in line with physical expectations and calibrations from binaries and clusters. However, two F-stars in the CoRoT field (HD 49933 and HD 181906) still necessitate high overshoot in the models. Due to short mode lifetimes, mode identification can be difficult in these stars. We demonstrate that an incongruence between the radial and non-radial modes drives the asteroseismic solution to extreme structures with highly-efficient CBM as an inevitable outcome. Understanding the cause of seemingly anomalous physics for such stars is vital for inferring accurate stellar parameters from TESS data with comparable timeseries length.

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Section: Modification Of the Composition Profile Through Cbmmentioning

confidence: 99%

Convective boundary mixing in low- and intermediate-mass stars – I. Core properties from pressure-mode asteroseismology

Angelou

Bellinger

Hekker

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…There is considerable evidence for additional mixing for Core Hydrogen Burning stars (CHB) on the upper main sequence, with a consensus that it extends to roughly 20% of the local pressure scale height (Schaller et al 1992;Herwig et al 1997;Weiss & Ferguson 2009;Miller Bertolami 2016;Ekström et al 2012). This is seen by the ability to reproduce the observations of the main sequence stars in open clusters (Maeder & Meynet 1991;Stothers & Chin 1992;Schroder et al 1997) and eclipsing binaries (Claret 2007;Stancliffe et al 2015;Higl & Weiss 2017).…”

Section: Core Hydrogen Burningmentioning

confidence: 99%

Impact of convective boundary mixing on the TP-AGB

Wagstaff

Bertolami

Weiß

2020

Monthly Notices of the Royal Astronomical Society

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The treatment of convective boundaries remains an important source of uncertainty within stellar evolution, with drastic implications for the thermally-pulsing stars on the Asymptotic Giant Branch (AGB). Various sources are taken as motivation for the incorporation of convective boundary mixing during this phase, from s-process nucleosynthesis to hydrodynamical models. In spite of the considerable evidence in favour of the existence of convective boundary mixing on the pre-AGB evolution, this mixing is not universally included in models of TP-AGB stars. The aim of this investigation is to ascertain the extent of convective boundary mixing, which is compatible with observations when considering full evolutionary models. Additionally, we investigate a theoretical argument that has been made that momentum-driven overshooting at the base of the pulse-driven convection zone should be negligible. We show that, while the argument holds, it would similarly limit mixing from the base of the convective envelope. On the other hand, estimations based on the picture of turbulent entrainment suggest that mixing is possible at both convective boundaries. We demonstrate that additional mixing at convective boundaries during core-burning phases prior to the thermally-pulsing Asymptotic Giant Branch has an impact on the later evolution, changing the mass range at which the third dredge-up and hot-bottom burning occur, and thus also the final surface composition. In addition, an effort has been made to constrain the efficiency of convective boundary mixing at the different convective boundaries, using observational constraints. Our study suggests a strong tension between different constraints that makes it impossible to reproduce all observables simultaneously within the framework of an exponentially decaying overshooting. This result calls for a reassessment of both the models of convective boundary mixing and the observational constraints.

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“…Stars with M > 0.8 M generally agree with theoretical models to within observational uncertainties. Lower mass stars, however, are often observed to have radii that are 5-15% larger than model predictions (López-Morales 2007; Morales et al 2008;Torres et al 2010;Kraus et al 2011;Higl & Weiss 2017;Cruz et al 2018;Kesseli et al 2018). There is observational and theoretical evidence to suggest that magnetic fields could be the cause (Chabrier et al 2007;Morales et al 2010;Feiden & Chaboyer 2013;MacDonald & Mullan 2017), due to interaction with the partially convective outer atmospheres and/or generation of cool starspots at polar latitudes.…”

Section: Introductionmentioning

confidence: 99%

The SDSS-HET Survey of Kepler Eclipsing Binaries. Description of the Survey and First Results

Mahadevan

Bender

Hambleton

et al. 2019

ApJ

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The Kepler mission has provided a treasure trove of eclipsing binaries (EBs), observed at extremely high photometric precision, nearly continuously for several years. We are carrying out a survey of ∼100 of these EBs to derive dynamical masses and radii with precisions of 3% or better. We use multiplexed near-infrared H band spectroscopy from the Sloan Digital Sky Survey-III and -IV APOGEE instrument and optical spectroscopy from the Hobby Eberly telescope High-Resolution Spectrograph to derive double-lined spectroscopic orbits and dynamical mass-ratios (q) for the EB sample, two of which we showcase in this paper. This orbital information is combined with Kepler photometry to derive orbital inclination, dynamical masses of the system component, radii and temperatures. These measurements are directly applicable for benchmarking stellar models that are integrating the next generation of improvements, such as the magnetic suppression of convection efficiency, updated opacity tables, and fine-tuned equations of state. We selected our EB sample to include systems with low-mass (M 0.8 M ) primary or secondary components, as well as many EBs expected to populate the relatively sparse parameter space below ∼ 0.5 M . In this paper, we describe our EB sample and the analysis techniques we are utilizing, and also present masses and radii for two systems that inhabit particularly underpopulated regions of mass-radius-period space: KIC 2445134 and KIC 3003991. Our joint spectrosopic and photometric analysis of KIC 2445134 (q = 0.411 ± 0.001) yields masses and radii of M A = 1.29 ± 0.03 M , M B = 0.53 ± 0.01 M , R A = 1.42 ± 0.01 R , R B = 0.510 ± 0.004 R , and a temperature ratio of T B /T A = 0.635 ± 0.001; our analysis of KIC 3003991 (q = 0.298 ± 0.006) yields M A = 0.74 ± 0.04 M , M B = 0.222 ± 0.007 M , R A = 0.84 ± 0.01 R , R B = 0.250 ± 0.004 R , and a temperature ratio of T B /T A = 0.662 ± 0.001.

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Testing stellar evolution models with detached eclipsing binaries

Cited by 59 publications

References 112 publications

Convective boundary mixing in low- and intermediate-mass stars – I. Core properties from pressure-mode asteroseismology

Convective boundary mixing in low- and intermediate-mass stars – I. Core properties from pressure-mode asteroseismology

Impact of convective boundary mixing on the TP-AGB

The SDSS-HET Survey of Kepler Eclipsing Binaries. Description of the Survey and First Results

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