Grids of stellar models including second harmonic and colors: solar composition (<i>Z</i>= 0.0172,<i>X</i>= 0.7024)

Yıldız, Mutlu

doi:10.1088/1674-4527/15/12/012

Cited by 8 publications

(7 citation statements)

References 45 publications

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“…Today, there are many theoretical stellar evolution models available. Notable examples include: Geneva Grids of Stellar Evolution Models (Schaller et al 1992;Schaerer et al 1993), Padova Database of Stellar Evolution Tracks (Girardi et al 2000;Marigo et al 2008;Bertelli et al 2008Bertelli et al , 2009Girardi et al 2010;Bressan et al 2012;Chen et al 2015), Yonsei-Yale Isochrones (Demarque et al 2004(Demarque et al , 2008 (Paxton et al 2011(Paxton et al , 2013(Paxton et al , 2015Dotter 2016;Choi et al 2016), others such as Pols et al (1998), Yıldız (2015), and more.…”

Section: Constraining Metallicity and Agementioning

confidence: 99%

Interrelated main-sequence mass–luminosity, mass–radius, and mass–effective temperature relations

Eker

Bakış

Bilir

et al. 2018

Monthly Notices of the Royal Astronomical Society

207

185

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Absolute parameters of 509 main-sequence stars selected from the components of detached-eclipsing spectroscopic binaries in the Solar neighbourhood are used to study mass-luminosity, mass-radius and mass-effective temperature relations (MLR, MRR and MTR). The MLR function is found better if expressed by a six-piece classical MLR (L ∝ M α ) rather than a fifth or a sixth degree polynomial within the mass range of 0.179 M/M ⊙ 31. The break points separating the mass-ranges with classical MLR do not appear to us to be arbitrary. Instead, the data indicate abrupt changes along the mass axis in the mean energy generation per unit of stellar mass. Unlike the MLR function, the MRR and MTR functions cannot be determined over the full range of masses. A single piece MRR function is calibrated from the radii of stars with M 1.5M ⊙ , while a second single piece MTR function is found for stars with M > 1.5M ⊙ . The missing part of the MRR is computed from the MLR and MTR, while the missing part of the MTR is computed from the MLR and MRR. As a result, we have interrelated MLR, MRR and MTR, which are useful in determining the typical absolute physical parameters of main-sequence stars of given masses. These functions are also useful to esc The Authors 2 Eker et al. timate typical absolute physical parameters from typical T ef f values. Thus, we were able to estimate the typical absolute physical parameters of mainsequence stars observed in the Sejong Open Cluster survey, based on that survey's published values for T ef f . Since typical absolute physical parameters of main sequence stars cannot normally be determined in such photometric surveys, the interrelated functions are shown to be useful to compute such missing parameters from similar surveys.

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Section: Constraining Metallicity and Agementioning

confidence: 99%

Interrelated main-sequence mass–luminosity, mass–radius, and mass–effective temperature relations

Eker

Bakış

Bilir

et al. 2018

Monthly Notices of the Royal Astronomical Society

207

185

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“…of the target stars, computed from νmaxT 0.5 eS , is plotted with respect to log(T eS ). The thin and thick solid lines represent ZAMS and TAMS lines taken from Yıldız (2015), respectively. HD 146233) were obtained from ground-based observations (Bedding et al 2010, Bedding et al 2007and Bazot et al 2012.…”

Section: Asteroseismic and Non-asteroseismic Properties Of Kepler Andmentioning

confidence: 99%

Fundamental properties ofKeplerandCoRoTtargets – III. Tuning scaling relations using the first adiabatic exponent

Yıldız

Orhan

Kayhan

2016

Mon. Not. R. Astron. Soc.

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So called scaling relations have the potential to reveal the mass and radius of solar-like oscillating stars, based on oscillation frequencies. In derivation of these relations, it is assumed that the first adiabatic exponent at the surface (Γ 1s ) of such stars is constant. However, by constructing interior models for the mass range 0.8-1.6 M ⊙ , we show that Γ 1s is not constant at stellar surfaces for the effective temperature range with which we deal. Furthermore, the well-known relation between large separation and mean density also depends on Γ 1s . Such knowledge is the basis for our aim of modifying scaling relations. There are significant differences between masses and radii found from modified and conventional scaling relations. However, comparison of predictions of these relations with the non-asteroseismic observations of Procyon A reveals that new scaling relations are effective in determining the mass and radius of stars. In the present study, solar-like oscillation frequencies of 89 target stars (mostly Kepler and CoRoT) were analysed. As well as two new reference frequencies (ν min1 and ν min2 ) found in the spacing of solar-like oscillation frequencies of stellar interior models, we also take into account ν min0 . In addition to the frequency of maximum amplitude, these frequencies have very strong diagnostic potential for determination of fundamental properties. The present study involves the application of derived relations from the models to the solar-like oscillating stars, and computes their effective temperatures using purely asteroseismic methods. There are in general very close agreements between effective temperatures from asteroseismic and non-asteroseismic (spectral and photometric) methods. For the Sun and Procyon A, for example, the agreement is almost total.

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“…Also plotted is log g mod with respect to T mod of the best-fitting models (filled circles). Thin and thick solid lines are for the ZAMS and TAMS lines, respectively, taken from Yıldız (2015).…”

Section: Modelling Strategy and χ 2 Methodsmentioning

confidence: 99%

Asteroseismic Investigation of 20 Planet and Planet-Candidate Host Stars

Kayhan,

Yıldız,

Orhan

2019

Preprint

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Planets and planet candidates are subjected to great investigation in recent years. In this study, we analyse 20 planet and planet-candidate host stars at different evolutionary phases. We construct stellar interior models of the host stars with the MESA evolution code and obtain their fundamental parameters under influence of observational asteroseismic and non-asteroseismic constraints. Model mass range of the host stars is 0.74-1.55 M ⊙ . The mean value of the so-called large separation between oscillation frequencies and its variation about the minima show the diagnostic potential of asteroseismic properties. Comparison of variations of model and observed large separations versus the oscillation frequencies leads to inference of fundamental parameters of the host stars. Using these parameters, we revise orbital and fundamental parameters of 34 planets and four planet candidates. According to our findings, radius range of the planets is 0.35-16.50 R ⊕ . The maximum difference between the transit and revised radii occurs for Kepler-444b-f is about 25 per cent.

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Grids of stellar models including second harmonic and colors: solar composition (Z= 0.0172,X= 0.7024)

Cited by 8 publications

References 45 publications

Interrelated main-sequence mass–luminosity, mass–radius, and mass–effective temperature relations

Interrelated main-sequence mass–luminosity, mass–radius, and mass–effective temperature relations

Fundamental properties ofKeplerandCoRoTtargets – III. Tuning scaling relations using the first adiabatic exponent

Asteroseismic Investigation of 20 Planet and Planet-Candidate Host Stars

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