Astron. J., 156, 37-37 (2018/July-1)
Li in open clusters: cool dwarfs in the young, subsolar-metallicity cluster M35 (NGC 2168).
ANTHONY-TWAROG B.J., DELIYANNIS C.P., HARMER D., LEE-BROWN D.B., STEINHAUER A., SUN Q. and TWAROG B.A.
Abstract (from CDS):
Hydra spectra of 85 G-K dwarfs in the young cluster M35 near the Li 6708 Å line region are analyzed. From velocities and Gaia astrometry, 78 are likely single-star members that, combined with previous work, produce 108 members with Teff ranging from 6150 to 4000 K as defined by multicolor, broadband photometry, E(B - V) = 0.20, and [Fe/H] = -0.15, though there are indications the metallicity may be closer to solar. The Lithium abundance A(Li) follows a well-delineated decline from 3.15 for the hottest stars to upper limits <=1.0 among the coolest dwarfs. Contrary to earlier work, M35 includes single stars at systematically higher A(Li) than the mean cluster relation. This subset exhibits higher VROT than the more Li-depleted sample and, from photometric rotation periods, is dominated by stars classed as convective (C); all others are interface (I) stars. The cool, high-Li rapid rotators (RRs) are consistent with models that simultaneously consider rapid rotation and radius inflation; RRs hotter than the Sun exhibit excess Li depletion, as predicted by the models. The A(Li) distribution with color and rotation period, when compared to the Hyades/Praesepe and the Pleiades, is consistent with gyrochronological analysis placing M35's age between the older M34 and younger Pleiades. However, the Pleiades display a more excessive range in A(Li) and rotation period than M35 on the low-Li, slow-rotation side of the distribution, with supposedly younger stars at a given Teff in the Pleiades spinning slower, with A(Li) reduced by more than a factor of four compared to M35.
© 2018. The American Astronomical Society. All rights reserved.
open clusters and associations: individual: NGC 2168 - stars: abundances
VizieR on-line data:
<Available at CDS (J/AJ/156/37): table1.dat table2.dat table3.dat>
Tables 1-3: [ADH2018] FNN (Nos F1-F11).
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