Y2 Isochrones with an Improved Core Overshoot Treatment

By P. Demarque, J. Woo, Yong-Cheol Kim, S. Yi. 2004

761 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/9427a9df6b4c5833b3b5c471cd94d1cc79cf68da

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In Astronomy and Astrophysics

1. D. Charbonneau
2. Timothy Morton
3. J. Southworth
4. J. Johnson
5. J. Winn
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Citations in the corpus

• THE APOKASC CATALOG: AN ASTEROSEISMIC AND SPECTROSCOPIC JOINT SURVEY OF TARGETS IN THE KEPLER FIELDS (2014, methodology): “2008) and the Padova group (Marigo et al. 2008; Girardi et al. 2000), the set of YY isochrones (Demarque et al. 2004), a grid constructed using the Yale Stellar Evolution Code (YREC; Demarque et al. 2008) and described by Gai et al. (2011) (we refer to this set as YREC), and another set of models…”
• THE KEPLER-10 PLANETARY SYSTEM REVISITED BY HARPS-N: A HOT ROCKY WORLD AND A SOLID NEPTUNE-MASS PLANET (2014, methodology): “…the asteroseismic stellar density ρ as measured by Fogtmann-Schulz et al. (2014), the Teff , and [Fe/H] with the Yonsei-Yale evolutionary tracks (Torres et al. 2012; Sozzetti et al. 2007; Demarque et al. 2004) and by performing the same chi-square minimization as in Santerne et al. (2011).”
• STELLAR DIAMETERS AND TEMPERATURES. III. MAIN-SEQUENCE A, F, G, AND K STARS: ADDITIONAL HIGH-PRECISION MEASUREMENTS AND EMPIRICAL RELATIONS (2013, methodology): “We derive ages and masses for stars in Table 3 by fitting the measured radii and temperatures to the Yonsei-Yale (Y 2) stellar isochrones (Demarque et al. 2004; Yi et al. 2003; Kim et al. 2002; Yi et al. 2001).”
• VLBA DETERMINATION OF THE DISTANCE TO NEARBY STAR-FORMING REGIONS. III. HP TAU/G2 AND THE THREE-DIMENSIONAL STRUCTURE OF TAURUS (2009, methodology): “A similar 5 Myr age difference is found for the models of Demarque et al. (2004) and D’Antona & Mazzitelli (1997): both predict ages slightly smaller than 1 Myr for HP Tau/G3, and somewhat larger than 5 Myr for HP Tau/G2.”
• A SEARCH FOR STARS OF VERY LOW METAL ABUNDANCE. VI. DETAILED ABUNDANCES OF 313 METAL-POOR STARS (2014, background): “To reduce the impact of this effect on the ionization balance between Fe i and Fe ii, in most stars we derive surface gravities (log g, in cgs units) from theoretical isochrones in the Y2 grid (Demarque et al. 2004).”
• FUNDAMENTAL PROPERTIES OF KEPLER PLANET-CANDIDATE HOST STARS USING ASTEROSEISMOLOGY (2013, neutral): “…(BaSTI; Pietrinferni et al. 2004), the Dartmouth Stellar Evolution Database (DSEP; Dotter et al. 2008), the Padova stellar evolution code (Marigo et al. 2008), the Yonsei–Yale isochrones (YY; Demarque et al. 2004), and the Yale Rotating Stellar Evolution Code (YREC; Demarque et al. 2008).”
• The Initial Mass Function of the Massive Star-forming Region NGC 3603 from Near-Infrared Adaptive Optics Observations (2007, methodology): “For the 1.7 − 2.6 M⊙ low-mass bin, in addition to the PS99 set, we apply a PMS model published by Siess et al. (2000, hereafter SDF00), and the Y 2 isochrones based on the revised Yale models (Yi et al. 2001; Demarque et al. 2004).”
• The Metal-poor Halo of the Andromeda Spiral Galaxy (M31) (2006, methodology): “Interpolating metallicities within a grid of the Padova models (Girardi et al. 2002) and the Yale-Yonsei models (Y2 - Demarque et al. 2004) give consistent values to those derived using the Vandenberg, Bergbusch, & Dowler (2005) models.”
• Exploring the Milky Way stellar disk - A detailed elemental abundance study of 714 F and G dwarf stars in the solar neighbourhood (2013, neutral): “Stellar ages were determined from a fine grid ofα-enhanced Yonsei-Yale (Y2) isochrones by Demarque et al. (2004), adopting [α/Fe] = 0 for [Fe/H] > 0, [α/Fe] = −0.3 × [Fe/H] for −1 ≤ [Fe/H] ≤ 0, and [α/Fe] = +0.3 for [Fe/H] < −1.”
• Variations on Debris Disks: Icy Planet Formation at 30-150 AU for 1-3 M☉ Main-Sequence Stars (2008, background): “During postYmain-sequence evolution, the star brightens considerably (e.g., Demarque et al. 2004) and develops a powerful stellar wind (e.g., Knapp &Morris1985 and references therein), melting icy objects in the inner disk and ejecting small grains throughout the disk.”
• Spectroscopic Properties of Cool Stars (SPOCS). I. 1040 F, G, and K Dwarfs from Keck, Lick, and AAT Planet Search Programs (2005, methodology): “In this section, we interpret our observed HR diagram, using of Y2 isochrones (version 2) from theoretical stellar evolution models (Demarque et al. 2004).”
• PLANETARY CANDIDATES OBSERVED BY KEPLER. III. ANALYSIS OF THE FIRST 16 MONTHS OF DATA (2012, methodology): “The resulting surface gravity, effective temperature, and metallicity are used to identify the best-matching Yonsei–Yale stellar evolution model (Demarque et al. 2004) as described above for the KIC parameter adjustments.”
• SPECTRAL PROPERTIES OF COOL STARS: EXTENDED ABUNDANCE ANALYSIS OF 1,617 PLANET-SEARCH STARS (2016, methodology): “The isochrone based values in Columns (38)-(42) were derived by combining the luminosity with our final Teff , [Fe/H], and [Si/H] and interpolating in a grid of Yonsei-Yale isochrones (Demarque et al. 2004).”
• The Initial-Final Mass Relation: Direct Constraints at the Low-Mass End (2007, methodology): “For both clusters, the ages determined from the VandenBerg, Bergbusch, & Dowler (2006) isochrones are consistent at the ∼10% level with those determined from either the Yale-Yonsei isochrones (Demarque et al. 2004) or the Padova group isochrones (Girardi et al. 2002).”
• HAT-P-11b: A SUPER-NEPTUNE PLANET TRANSITING A BRIGHT K STAR IN THE KEPLER FIELD (2009, methodology): “On the other hand, the Yonsei-Yale stellar evolution models (Yi et al. 2001; Demarque et al. 2004) indicate (V − I)YY,expect = 0.98 ± 0.03 for a star with Teff⋆ ∼ 4850K (based on the SME results).”
• HD 147506b: A Supermassive Planet in an Eccentric Orbit Transiting a Bright Star (2007, methodology): “For this we used the Y2 models by Yi et al. (2001) and Demarque et al. (2004), and explored a wide range of ages to find all models consistent with Teff , MV , and [Fe/H] within the observational errors.”
• Chemical Similarities Between Galactic Bulge And Local Thick Disk Red Giant Stars (2008, methodology): “In addition, Yonsei-Yale (Demarque et al. 2004) and Padova isochrones (da Silva et al. 2006) were employed to determine evolutionary gravities.”