PARSEC V2.0: Stellar tracks and isochrones of low- and intermediate-mass stars with rotation

Nguyen, C.T.; Costa, Guglielmo; Girardi, L.; Volpato, Guglielmo; Bressan, A.; Chen, Y.; Marigo, Paola; Fu, X.; Goudfrooij, Paul

doi:10.1051/0004-6361/202244166

Cited by 70 publications

(41 citation statements)

References 112 publications

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“…isochrones (Bressan et al 2012;Nguyen et al 2022) corresponding to ages of 300, 400, and 500 Myr, roughly the range of ages quoted for Stock 2 in the literature.…”

Section: Target Selection and Color-magnitude Diagramsupporting

confidence: 76%

Chemically Peculiar Stars in the Open Cluster Stock 2

Casamiquela¹,

Gebran²,

Agüeros³

et al. 2022

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The recently rediscovered open cluster Stock 2, located roughly 375 pc away and about 400 Myr old, has the potential to be an exciting new testbed for our understanding of stellar evolution. We present results from a spectroscopic campaign to characterize stars near the cluster’s main-sequence turnoff; our goal is to identify candidate chemically peculiar stars among the cluster’s A stars. We obtained échelle spectra for 64 cluster members with ESPaDOnS on the 3.6 m Canada–France–Hawaii Telescope, Maunakea Observatory, USA, and for six stars with SOPHIE on the 1.93 m telescope at the Observatoire de Haute-Provence, France. We complemented these new observations with those of 13 high-mass cluster members from the HARPS-N archive; our overall sample is of 71 stars. We derived the fundamental parameters (T eff, log g , [M/H]) as well as v e sin i for our sample using the sliced inverse regression technique, and then used iSpec to derive individual abundances of 12 chemical species. With these abundance determinations, we identified nine A stars with anomalous levels of Sc, Ca, and other metallic lines. Follow-up observations of these Am candidates with a known age can transform them into benchmarks for evolutionary models that include atomic diffusion and help build a better understanding of the complex interactions between macroscopic and microscopic processes in stellar interiors.

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“…isochrones (Bressan et al 2012;Nguyen et al 2022) corresponding to ages of 300, 400, and 500 Myr, roughly the range of ages quoted for Stock 2 in the literature.…”

Section: Target Selection and Color-magnitude Diagramsupporting

confidence: 76%

Chemically Peculiar Stars in the Open Cluster Stock 2

Casamiquela¹,

Gebran²,

Agüeros³

et al. 2022

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“…To further investigate the evolution of this system, we analyzed the growth rate of the He core of stars with different masses at the cluster metallicity extracted from the PARSEC v2.0 database (Costa et al 2019a(Costa et al , 2019bNguyen et al 2022). Assuming the cluster age of 13.25 ± 0.5 Gyr (Dotter et al 2010), the sum of the companion cooling age and proto-WD age suggests that this system experienced the end of the mass transfer phase (i.e., Roche lobe detachment) when the cluster was 11.9 ± 0.5 Gyr old.…”

Section: Comparison With Binary Evolution Modelsmentioning

confidence: 99%

“…The posterior distribution is shown in Figure 6, and the results based on the 16th, 50th, and 84th percentiles show that NGC 6652B is likely an NS with a standard mass of 1.44 ± 0.06 M e in a binary seen with a large inclination angle. In fact, the probability (Costa et al 2019a(Costa et al , 2019bNguyen et al 2022). The black dashed curve and the light-orange shaded area represent the values for an age of 11.9 ± 0.5 Gyr, corresponding to the cluster age at the epoch of Roche lobe detachment.…”

Section: Constraints On the Ns Massmentioning

confidence: 99%

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A Young White Dwarf Orbiting PSR J1835−3259B in the Bulge Globular Cluster NGC 6652

Chen

Cadelano

Pallanca

et al. 2023

ApJ

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We report on the discovery of the companion star to the millisecond pulsar PSR J1835−3259B in the Galactic globular cluster NGC 6652. Taking advantage of deep photometric archival observations acquired through the Hubble Space Telescope in near-UV and optical bands, we identified a bright and blue object at a position compatible with that of the radio pulsar. The companion is located along the helium-core white dwarf cooling sequence, and the comparison with binary evolution models provides a mass of 0.17 ± 0.02 M ⊙, a surface temperature of 11,500 ± 1900 K, and a very young cooling age of only 200 ± 100 Myr. The mass and the age of the companion are compatible with a progenitor star of about 0.87 M ⊙, which started transferring mass to the primary during its evolution along the subgiant branch and stopped during the early red giant branch phase. Combining together the pulsar mass function and the companion mass, we found that this system is observed at an almost edge-on orbit and hosts a neutron star with a mass of 1.44 ± 0.06 M ⊙, thus suggesting a highly nonconservative mass accretion phase. The young age of the WD companion is consistent with the scenario of a powerful, relatively young MSP indicated by the earlier detection of gamma-rays from this system.

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“…We also show 5 Gyr, solar-metallicity isochrones from two models. We calculate the MIST isochrone (Choi et al 2016) using the MIST web interface 3 and the PARSEC isochrone (Nguyen et al 2022) using the PARSEC CMD input form. 4 The radius inflation of observed M dwarfs in eclipsing binaries relative to theoretical model predictions has been discussed extensively in past works (e.g., Torres 2013).…”

Section: Comparison With the Literaturementioning

confidence: 99%

G 68-34: A Double-lined M-dwarf Eclipsing Binary in a Hierarchical Triple System

Pass

Charbonneau

2023

ApJ

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Using high-resolution spectra from the Tillinghast Reflector Echelle Spectrograph and photometry from sector 56 of the Transiting Exoplanet Survey Satellite, we report that the nearby M dwarf G 68-34 is a double-lined eclipsing binary. The pair is spin–orbit synchronized with a period of 0.655 days. The light curve shows significant spot modulation with a larger photometric amplitude than that of the grazing eclipses. We perform a joint fit to the spectroscopic and photometric data, obtaining masses of 0.3280 ± 0.0034M ⊙ and 0.3207 ± 0.0036M ⊙ and radii of 0.345 ± 0.014R ⊙ and 0.342 ± 0.014R ⊙ after marginalizing over unknowns in the starspot distribution. This system adds to the small but growing population of fully convective M dwarfs with precisely measured masses and radii that can be used to test models of stellar structure. The pair also has a white-dwarf primary at 9″ separation, with the system known to be older than 5 Gyr from the white-dwarf cooling age. The binarity of G 68–34 confirms our hypothesis from Pass et al.: in that work, we noted that G 68-34 was both rapidly rotating and old, highly unusual given our understanding of the spin-down of M dwarfs, and that a close binary companion may be responsible.

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PARSEC V2.0: Stellar tracks and isochrones of low- and intermediate-mass stars with rotation

Cited by 70 publications

References 112 publications

Chemically Peculiar Stars in the Open Cluster Stock 2

Chemically Peculiar Stars in the Open Cluster Stock 2

A Young White Dwarf Orbiting PSR J1835−3259B in the Bulge Globular Cluster NGC 6652

G 68-34: A Double-lined M-dwarf Eclipsing Binary in a Hierarchical Triple System

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