J/AJ/106/1059ivo://CDS.VizieR/J/AJ/106/1059doi:10.26093/cds/vizier.51061059CDSSoderblom D.R.Jones B.F.Balachandran S.Stauffer J.R.,Duncan D.K.Fedele S.B.Hudon J.D.2023-04-06T16:50:03Z1999-03-02T10:00:06ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frchemical-abundancesopen-star-clustersWe report new measurements of lithium in more than 100 Pleiades F, G, and K dwarfs. Abundances were determined from spectrum synthesis fits to the data as well as from use of new curves of growth for the Li 6708 A feature (presented in an Appendix). We confirm the intrinsic spread in lithium abundance within the Pleiades seen by Duncan & Jones (1983ApJ...271..663D), but we establish more observational constraints on Li in this cluster: First, for stars near 1.0M_sun_ [about 0.60 to 0.75 in (B-V)0], the scatter in the relation between log N(Li) (defined as N(Li)) and T(eff) is consistent with our observational uncertainty. That means that most late-F and early-G dwarfs in the Pleiades are consistent with the tight N(Li) versus mass relation seen in the Hyades in the same mass range. Second, at (B-V)0~0.8 (M~0.9M_sun_), large and real star-to-star differences in N(Li) appear. The range in N(Li) at (B-V)0~0.8 is about 1dex, and grows to as much as 1.5dex for less massive stars. Third, the most Li-rich stars have abundances at or near the primordial level for Population I (N(Li)~3.2), and none exceed that level by a significant amount. Fourth, at any given color the stars that rotate fastest have the most Li and have the strongest chromospheric activity. We consider the ways in which an apparent spread in N(Li) could arise from an intrinsically tight N(Li)-mass relation and conclude that the spread is probably real and is not an artifact of line formation conditions or inhomogeneous atmospheres on the stars. It is possible to produce large apparent changes in N(Li) by covering a significant fraction of a star's surface with cooler regions ("spots"), but doing so has other ramifications that conflict with the observations. Some current models lead to a spread in N(Li) in which the fastest rotators (those that have lost the least angular momentum) have the most Li, and that mechanism may account for what is seen. A comparison of the Pleiades to the Alpha Persei cluster shows that most Alpha Persei stars have Li abundances comparable to their Pleiades counterparts, but there is a significant fraction (about 30%) of Alpha Persei stars that lie below the Pleiades in N(Li) by 1dex or more. Some of these anomalous stars have even less Li than Hyades stars of the same T(eff). If these stars are bona fide Alpha Persei members (and they probably are), their Li abundances strain our understanding of Li depletion. The Pleiades, considered together with Alpha Persei and the Hyades, shows that stars with [Fe/H]>=0.0 and which are more massive than about 1.25M_sun_ do not deplete Li prior to reaching main the sequence. Moreover, solar-abundance stars ([Fe/H]~0.0) with M>~1.1M_sun_ do not experience pre-main-sequence depletion either. Pleiades dwarfs near T(eff)=6700K show evidence of being depleted in Li, indicating that an incipient Li "chasm" is present even at an age of 70Myr.1993AJ....106.1059Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/106/1059CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/AJ/106/1059https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/AJ/106/1059http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/AJ/106/1059https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/AJ/106/1059https://vizier.iucaa.in/viz-bin/votable?-source=J/AJ/106/1059http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/AJ/106/1059GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/AJ/106/1059/table1Observations of Lithium in Pleiades F, G, and K dwarfsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintfgkfgk number from Soderblom et al. (1993ApJS...85..315S) (hereafter SSHJ)meta.idcharnameHertzsprung (H II) designation. A "P" prefix denotes a Pels star.meta.id;meta.maincharSpSpectral typesrc.spTypechar(B-V)0Dereddened (B-V)magphot.color;em.opt.B;em.opt.Vfloatu_(B-V)0Uncertainty flag on (B-V)0meta.code.errorcharTeffEffective temperatureKphys.temperature.effectiveintl_vsiniLimit flag on vsinimeta.code.errorcharvsini? Rotational velocitykm/sphys.veloc.rotatfloatnullableu_vsiniuncertainty flag on vsinimeta.code.errorcharn_vsini[S ] 'S' indicating a double-lined spectroscopic binary whose vsini values are given in table2 of SSHJ (SB2).meta.notecharlog(RHalpha)[]? Ratio of the Halpha flux to the stellar bolometric flux, log R(Halpha) from SSHJphot.flux;arith.ratiofloatnullablelog(R8542)[]? Ratio of the 8542 A Ca II line flux to the stellar bolometric flux, logR(8542) from SSHJphot.flux;arith.ratiofloatnullableW7699[]? Equivalent width of K I 7699A linepmspect.line.eqWidthfloatnullableW6717[]? Equivalent width of Ca I 6717 A linepmspect.line.eqWidthfloatnullablen_W6717Note on W6717. See note (1)meta.notecharl_W6708Limit flag on W6708meta.code.errorcharW6708Equivalent width of Li I 6708 A line, corrected for Fe I 6707.441.pmspect.line.eqWidthfloatu_W6708Uncertainty flag on W6708meta.code.errorcharn_W6708Note on W6708. See note (1)meta.notecharqSource and quality code (2)meta.code.qualcharl_log(N(Li))Limiting character for lithium abundancemeta.code.errorcharlog(N(Li))Abundance of lithium (scale logN(H)=12)phys.abundfloatu_log(N(Li))Uncertainty flag on log(N(Li))meta.code.errorcharJ/AJ/106/1059/table2*Lithium abundances for the 6708 A featurerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlog(W6708)Equivalent width of Li 6708 linelog(0.1pm)spect.line.eqWidthfloatlogN(Li)1Li abundance for Teff = 4000 Kphys.abundfloatlogN(Li)2Li abundance for Teff = 4250 Kphys.abundfloatlogN(Li)3Li abundance for Teff = 4500 Kphys.abundfloatlogN(Li)4[]? Li abundance for Teff = 4750 Kphys.abundfloatnullablelogN(Li)5[]? Li abundance for Teff = 5000 Kphys.abundfloatnullablelogN(Li)6[]? Li abundance for Teff = 5250 Kphys.abundfloatnullablelogN(Li)7[]? Li abundance for Teff = 5500 Kphys.abundfloatnullablelogN(Li)8[]? Li abundance for Teff = 5750 Kphys.abundfloatnullablelogN(Li)9[]? Li abundance for Teff = 6000 Kphys.abundfloatnullablelogN(Li)10[]? Li abundance for Teff = 6250 Kphys.abundfloatnullablelogN(Li)11[]? Li abundance for Teff = 6500 Kphys.abundfloatnullableJ/AJ/106/1059/table3*Lithium abundances for the 6104 A featurerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlog(W6708)Equivalent width of Li 6708 linelog(0.1pm)spect.line.eqWidthfloatlogN(Li)1Li abundance for Teff = 4000 Kphys.abundfloatlogN(Li)2Li abundance for Teff = 4250 Kphys.abundfloatlogN(Li)3Li abundance for Teff = 4500 Kphys.abundfloatlogN(Li)4[]? Li abundance for Teff = 4750 Kphys.abundfloatnullablelogN(Li)5[]? Li abundance for Teff = 5000 Kphys.abundfloatnullablelogN(Li)6[]? Li abundance for Teff = 5250 Kphys.abundfloatnullablelogN(Li)7[]? Li abundance for Teff = 5500 Kphys.abundfloatnullablelogN(Li)8[]? Li abundance for Teff = 5750 Kphys.abundfloatnullablelogN(Li)9[]? Li abundance for Teff = 6000 Kphys.abundfloatnullablelogN(Li)10[]? Li abundance for Teff = 6250 Kphys.abundfloatnullablelogN(Li)11[]? Li abundance for Teff = 6500 Kphys.abundfloatnullable