Issue |
A&A
Volume 515, June 2010
|
|
---|---|---|
Article Number | L3 | |
Number of page(s) | 7 | |
Section | Letters | |
DOI | https://doi.org/10.1051/0004-6361/200913047 | |
Published online | 15 June 2010 |
LETTER TO THE EDITOR
Observational evidence for a broken Li Spite plateau and mass-dependent Li depletion
,![[*]](/icons/foot_motif.png)
J. Meléndez1 - L. Casagrande2 - I. Ramírez2 - M. Asplund2 - W. J. Schuster3
1 - Centro de Astrofísica da Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal
2 -
Max Planck Institute for Astrophysics, Postfach 1317, 85741 Garching, Germany
3 -
Observatorio Astronómico Nacional, Universidad Nacional Autónoma de México, Ensenada, B.C., CP 22800, Mexico
Received 31 July 2009 / Accepted 12 May 2010
Abstract
We present NLTE Li abundances for 88 stars in the metallicity range
-3.5 < [Fe/H] < -1.0. The effective temperatures are
based on the infrared flux method with improved E(B-V) values obtained mostly from interstellar Na I D lines.
The Li abundances were derived through MARCS models and
high-quality UVES+VLT, HIRES+Keck and FIES+NOT spectra, and
complemented with reliable equivalent widths from the literature. The
less-depleted stars with [Fe/H] < -2.5 and [Fe/H] >
-2.5 fall into two well-defined plateaus of
=
and
=
,
respectively. We show that the two plateaus are flat, unlike previous
claims for a steep monotonic decrease in Li abundances with
decreasing metallicities. At all metallicities we uncover a
fine-structure in the Li abundances of Spite plateau stars, which
we trace to Li depletion that depends on both metallicity and
mass.
Models including atomic diffusion and turbulent mixing seem to
reproduce the observed Li depletion assuming a primordial
Li abundance
= 2.64, which agrees well with current predictions (
= 2.72)
from standard Big Bang nucleosynthesis. Adopting the Kurucz
overshooting model atmospheres increases the Li abundance by
+0.08 dex to
= 2.72, which perfectly agrees with BBN+WMAP.
Key words: nuclear reactions, nucleosynthesis, abundances - cosmology: observations - stars: abundances - stars: Population II
1 Introduction
One of the most important discoveries in the study of the chemical
composition of stars was made in 1982 by Monique and François Spite,
who found an essentially constant Li abundance in warm metal-poor
stars (Spite & Spite 1982),
a result interpreted as a relic of primordial nucleosynthesis.
Due to its cosmological significance, there have been many studies
devoted to Li in metal-poor field stars (e.g., Ryan et al. 1999; Meléndez & Ramírez 2004, hereafter MR04;
Boesgaard et al. 2005, hereafter B05; Charbonnel & Primas 2005; Asplund et al. 2006, hereafter A06; Shi et al. 2007, hereafter S07; Bonifacio et al. 2007, hereafter B07; Hosford et al. 2009; Aoki et al. 2009; Sbordone et al. 2010, hereafter S10), with observed Li abundances at the lowest metallicities ([Fe/H] -3) from
= 1.94 (B07) to
= 2.37 (MR04).
A primordial Li abundance of
= 2.72
-0.06+0.05 is predicted (Cyburt et al. 2008; see also Steigman 2009; Coc & Vangioni 2010) with the theory of big bang nucleosynthesis (BBN) and the baryon density obtained from WMAP data (Dunkley et al. 2009),
which is a factor of 2-6 times higher than the Li abundance
inferred from halo stars. There have been many theoretical studies on
non-standard BBN trying to explain the cosmological Li discrepancy
by exploring the frontiers of new physics (e.g. Coc et al. 2009; Iocco et al. 2009; Jedamzik & Pospelov 2009; Kohri & Santoso 2009).
Alternatively, the Li problem could be explained by a reduction of
the original Li stellar abundance due to internal processes (i.e.,
by stellar depletion). In particular, stellar models including
atomic diffusion and mixing can deplete a significant fraction of the
initial Li content (Richard et al. 2005; Piau 2008),
although such models depend on largely unconstrained free parameters.
On the other hand, it is not easy to reconcile the lack of observed
abundance scatter in the Spite plateau with substantial
Li depletion (e.g. Ryan et al. 1999;
A06). Due to the uncertainties in the Li abundances and to the
small samples available, only limited comparisons of models of
Li depletion with stars in a broad range of mass and metallicities
have been performed (e.g., Pinsonneault et al. 2002; B05).
The observed scatter in derived Li abundances in previous studies of
metal-poor stars can be as low as 0.03 dex (e.g. Ryan
et al. 1999;
A06), fully consistent with the expected observational errors. Yet,
for faint stars observational errors as high as 0.2 dex have
been reported (e.g., Aoki et al. 2009).
In order to provide meaningful comparisons with stellar depletion
models, precise Li abundances for a large sample of stars are
needed. Here we present such a study for the first time for a large
sample of metal-poor stars
(-3.5 < [Fe/H] < -1.0) with masses in a
relatively broad mass range (0.6-0.9 ).
2 Stellar sample and atmospheric parameters
The sample was initially based on the 62 stars analysed by MR04. We added stars with published equivalent width (EW) measurements based on high-quality observations (Sect. 3), and included also stars for which we could obtain EW
Li measurements from UVES+VLT, HIRES+Keck and FIES+NOT spectra
(either from our own observations or from the archives). The resolving
power of the different instruments used ranges from 45 000
to 110 000, and the S/N is typically >100. Some measurements
taken from the literature were obtained with lower resolving power (
35 000), or high resolving power (R
50 000) but lower S/N. When necessary we averaged several
measurements in order to decrease the errors. The stars for which we could not obtain EW better than
5% were discarded, with a few exceptions (see Sect. 3). Our adopted log g
values and metallicities [Fe/H] are mean values (after discarding
outliers) taken from the compilation of stellar parameters by Meléndez
(in preparation), who has updated the metallicity catalogue of
Cayrel de Strobel et al. (2001)
from 4918 entries to more than 14 000. We only keep stars with at
least two previous spectroscopic analyses, so that their metallicities
and surface gravities have been confirmed at least by one other study.
The sample has 88 stars with stellar parameters
K,
and
.
We obtained effective temperatures (
)
by a new implementation (Casagrande et al. 2010, hereafter C10; see also Casagrande et al. 2006) of the infrared flux method (IRFM). In our previous work on Li abundances in metal-poor stars (MR04),
was obtained from the IRFM implementation by Ramírez & Meléndez (2005), relying on the calibration of the bolometric correction by Alonso et al. (1995),
which contains only a few low-metallicity stars; thus, for very
metal-poor turn-off stars, it is not well defined and may
introduce systematic errors. Indeed, C10 have found that below
[Fe/H]
-2.5, the Ramírez & Meléndez (2005)
go from being too cool by
K at [Fe/H] = -2.5 to too hot by
K at [Fe/H] = -3.5.
Our new IRFM implementation determines the bolometric flux from observed broad-band photometry
(BVRIJHK), thus representing an important improvement over the
obtained by Ramírez & Meléndez (2005). Furthermore, the zero point of our
scale has been carefully checked for accuracy using solar twins (their average
matching the solar one within a few K), spectral energy
distributions measured with HST for a metal-rich star with planet and a
metal-poor turn-off star, and stars with interferometric angular
diameters (for which our IRFM
and fluxes result in angular diameters only 0.6
1.7% smaller, corresponding to
18
50 K).
Thus, contrary to most previous studies, the uncertainty of our
absolute Li abundances is not dominated by the unknown zero point
of the adopted
scale.
In order to obtain
values with IRFM, one needs good estimates of E(B-V)
to properly correct the photometric data. In our previous work we
used extinction maps (see Sect. 4 in Meléndez et al. 2006a, hereafter M06), but in order to achieve a very high precision (
0.005 mag),
we must rely on other methods. Thanks to the large radial velocity of
most metal-poor stars, the interstellar Na I D lines can be used to obtain this precision. We employed this technique (Alves-Brito et al. 2010) when high-resolution spectra were available (
72% of the cases), otherwise we used extinction maps (M06). Our adopted E(B-V) values are shown in Fig. 1 and have median errors of 0.003
0.002 mag, implying errors in
of
K. Adding in errors in photometry, bolometric flux, log g and [Fe/H], we estimate a typical total internal error in
of
K
.
![]() |
Figure 1: Adopted E(B-V) values vs. [Fe/H]. Filled squares are values based on NaD lines and open squares on reddening maps. |
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We obtained stellar masses from the -enhanced Y2 isochrones (Demarque et al. 2004). We interpolated a fine grid of models with a step
[Fe/H] = 0.02 dex and adopting [
/Fe] = 0 for [Fe/H]
0, [
/Fe] = -0.3
[Fe/H] for -1 < [Fe/H] < 0, and [
/Fe] = +0.3 for [Fe/H]
-1
. At a given metallicity, we searched for all solutions allowed by the error bars in
,
Hipparcos parallaxes (reliably available for 2/3 of the sample)
and [Fe/H], adopting the median value in age and mass, and the
standard deviation of the solutions is adopted as the error. We also
used the mean log g values
found in the literature to estimate another set of masses and ages. The
masses obtained by both methods agree very well (median difference
[Hipparcos - literature] of -0.001
). The weighted averages of both results were adopted. We find typical ages of
11 Gyr and masses in the range of 0.6-0.9
.
In a few cases the adopted stellar parameters resulted in low
ages (<6 Gyr), probably due to errors in log g.
In those cases we estimated masses adopting an
age = 11 Gyr, but the choice of age does not affect our
conclusions (e.g.,
age = +1 Gyr results in
mass = -0.007
for a dwarf with [Fe/H] = -2 and
6300 K).
3 Li abundance analysis
The LTE Li abundances were obtained with our code (A06) with MARCS (Gustafsson et al. 2008) models and the 2002 version of MOOG (Sneden 1973) with Kurucz overshooting (Castelli et al. 1997)
models (which have improved overshooting with respect to earlier models
that showed several problems described in van't Veer-Menneret &
Megessier 1996). Both model atmospheres give similar Li abundances except for a zero-point difference of 0.08 dex (Kurucz overshooting - MARCS).
According to MR04 the difference in
between Kurucz overshooting and no-overshooting models is also
0.08 dex, so Kurucz no-overshooting models give similar
as the MARCS models. The results presented herein will be based on
the MARCS models, because the overshoot option implemented by
Kurucz is not supported by 3D hydrodynamical model atmospheres
(Asplund et al. 1999; see also Heiter et al. 2002);
we will nevertheless mention the implication of using Kurucz
overshooting models for completeness. We adopt the 1D non-LTE
corrections by Lind et al. (2009a), which are based on the most recent radiative and collisional data (Barklem et al. 2003).
The difference between LTE and non-LTE is relatively constant for our
stars so that similar conclusions
would have been obtained assuming LTE, yet, for an accurate analysis
NLTE must be taken into account because it affects the absolute level
of the Spite plateau. For metal-poor ([Fe/H] < -1) stars
with
> 6000 K the typical NLTE correction is -0.06
0.01 dex.
We measured the EW of the Li feature at 6707.8 Å
using UVES+VLT, HIRES+Keck and FIES+NOT high-resolution spectra, from
which we obtain typical errors in EW of 0.7 mÅ, which includes
uncertainties in continuum placement. We complemented our measurements with data from the literature
(B05; A06; B07; S07; Asplund & Meléndez 2008, hereafter AM08; S10). An important improvement with respect to our previous work is that now we select stars with errors in EW below 5% (typically 2-3%),
instead of the 10% limit adopted in MR04. The only exceptions are the
cool dwarfs HD 64090 and BD+38 4955, which are severely
depleted in Li and have EW errors of 8% and 10%,
respectively, and the very metal-poor stars (B07) BPS CS29518-0020
(5.2%) and BPS CS29518-0043 (6.4%), which were kept due to their
low metallicity.
The main sources of error are the uncertainties in equivalent widths and
,
which in our work have typical values of only 2.3%
and 50 K, implying abundance errors of 0.010 dex and
0.034 dex, respectively, and a total error in
of
0.035 dex. This low error in
is confirmed by the star-to-star scatter of the Li plateau stars, which have similar low values (e.g.
= 0.036 dex
for [Fe/H] < -2.5, see below). Our Li abundances
and stellar parameters are given in Table 1 (available in the online edition).
![]() |
Figure 2:
Li abundances vs.
|
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4 Discussion
4.1 The Teff cutoff of the Spite plateau
Despite the fact that Li depletion depends on mass (e.g. Pinsonneault et al. 1992), this variable has been ignored by most previous studies. Usually a cutoff in

At a given mass, the
of metal-poor stars has a strong metallicity-dependence (e.g. Demarque et al. 2004). As shown in Figs. 11, 12 of M06, the
of turnoff stars increases for decreasing metallicities. Hence, a metallicity-independent cutoff in
may be an inadequate way to exclude low-mass Li-depleted stars from the Spite plateau. As show in Fig. 2, where
in different metallicity bins is shown as a function of
,
stars with lower
in a given metallicity regime are typically the stars with the lowest
Li abundances, an effect that can be seen even in the sample
stars with the lowest metallicities ([Fe/H]
-3).
This is ultimately
so because the coolest stars are typically the least massive, and
therefore have been more depleted in Li (see Sect. 4.3).
![]() |
Figure 3:
Li abundances for stars with
|
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In Fig. 3 we show the Li
abundance for cutoffs =5700 K (open circles), 6100 K (filled
squares) and 6350 K (filled triangles). Using a hotter cutoff is
useful to eliminate the most Li-depleted stars at low metallicities,
but it removes from the Spite plateau stars with
[Fe/H] > -2. Imposing a hotter
cutoff
at low metallicities and a cooler cutoff at high metallicities
eliminates the most Li-depleted stars at low metallicities, but keeps
the most metal-rich stars in the Spite plateau. We propose such a
metallicity-dependent cutoff below.
4.2 Two flat Spite plateaus
Giving the shortcomings of a constant
cutoff, we propose an empirical cutoff of
= 5850-180
[Fe/H]. The stars above this cutoff are shown as stars in the bottom panel of Fig. 3.
Our empirical cutoff excludes only the most severely Li-depleted stars,
i.e., the stars that remain in the Spite plateau may still be affected
by depletion. The less Li-depleted stars in the bottom panel of
Fig. 3 show two well-defined groups separated at [Fe/H]
-2.5
(as shown below, this break represents a real discontinuity),
which have essentially zero slopes (within the error bars) and very low
star-to-star scatter in their Li abundances. The first group has
-2.5
[Fe/H] < -1.0 and
= 2.272 (
= 0.051) dex
and a slope of 0.018
0.026, i.e., flat within the uncertainties. The second group is more metal poor ([Fe/H] < -2.5) and has
= 2.184 dex (
) dex. The slope of this second group is also zero (-0.008
0.037). Adopting a more conservative exponential cutoff obtained from Y2 isochrones (Demarque et al. 2004), which for a 0.79
star can be fit by
= 6698-2173
,
we
would also recover a flat Spite plateau, although only stars with
[Fe/H] > -2.5 are left using this more restrictive
cut-off. Thus, the flatness of the Spite plateau is independent of
applying a linear or an exponential cutoff.
Adopting a constant cutoff in
we also find flat plateaus. For example adopting a cutoff of
> 6100 K (filled squares in Fig. 3) we find in the most metal-rich plateau ([Fe/H]
-2.5) no trend between Li and [Fe/H] (slope = 0.019
0.025, Spearman rank correlation coefficient
= 0.1 and a probability of 0.48 (i.e., 48%) of a correlation arising by pure chance for [Fe/H]
-2.5),
while for the most metal-poor plateau ([Fe/H] < -2.5) we
also do not find any trend within the errors (slope = 0.058
0.072,
= 0.2 and 41% probability of a spurious correlation). Using a
hotter cutoff (
> 6350 K, filled triangles in Fig. 3) we obtain also two flat plateaus with
slope = -0.040
0.063 (
= -0.2, probability =60%) for [Fe/H]
-2.5 and slope = 0.008
0.035 (
= 0.1, probability =68%) for [Fe/H] < -2.5.
![]() |
Figure 4:
a) Filled circles show the slope/ |
Open with DEXTER |
In Fig. 4 we demonstrate that the break at [Fe/H] -2.5 is statistically significant. In panel (a) the slope/
in the
vs. [Fe/H] plot for the range
< [Fe/H] < -1.0 are shown as filled circles, where
varies within [-3.50, -1.25]. For
-2.5, the slope is insignificant (
3
), and only when stars with [Fe/H] < -2.5 are included a measurable slope is forced in the
vs. [Fe/H] relation. The opposite test is shown by open circles, where we show slope/
for the range -3.25 < [Fe/H] <
,
where
changes from [-3.00, -1.00]. For
< -2.5 the slope is negligible (
3
), and only when stars with [Fe/H]
-2.5 are included, a slope is produced between
and [Fe/H]. The correlation coefficient
and the probability of a correlation between
and [Fe/H] by pure chance are shown in panel (b). Again, this plot shows that no correlation between
and [Fe/H] exists within the two groups (-3.5 < [Fe/H] < -2.5 and -2.5
[Fe/H]
-1.0), and that only when stars between the two groups are mixed, significant (probability
0) correlations of
with [Fe/H] are generated. Systematically lower E(B-V) values (by
0.03 mag) in the most metal-poor plateau ([Fe/H] < -2.5) could produce a more Li-depleted plateau.
However, those E(B-V) values (Fig. 1) are actually slightly higher (
0.007 mag, i.e.,
33 K) than those for [Fe/H]
-2.5
(mainly due to a high number of unreddened nearby more metal-rich
stars), thus not explaining the existence of two different plateaus.
Previous claims of a steep monotonic decrease in Li abundance with decreasing metallicity (e.g. Ryan et al. 1999; A06; B07; Hosford et al. 2009)
are probably due to the mix of stars from the two different groups,
forcing a monotonic dependence with metallicity. Our large sample of
homogeneous and precise Li abundances that covers a broad
metallicity range (-3.5 < [Fe/H] < -1.0) does
not support these claims. Nevertheless, a hint of two different
groups in the Spite plateau was already found by A06, who found a
change in the slope of the Spite plateau at [Fe/H] -2.2.
Also, in the combined A06+B07 sample (Fig. 7 of B07),
there are two different groups: stars with [Fe/H]
-2.6 have
> 2.2, while stars with [Fe/H]
-2.6 have
< 2.2.
Although in the study by MR04 a flat Spite plateau is found in the
range -3.4 < [Fe/H] < -1, this is due to the
overestimation of
below [Fe/H] < -2.5, thus overestimating
at low metallicities and forcing a flat plateau from [Fe/H] = -3.4 to -1.
4.3 Correlation between Li and mass
Models of Li depletion predict that the least massive stars are the
most depleted in Li, but due to the limitations of previous samples,
these predictions have not been thoroughly tested at different
metallicity regimes in metal-poor stars. In Fig. 5
we show our Li abundances as a function of stellar mass for
different metallicity ranges. As can be seen,
the Li plateau stars have a clear dependence with mass for
all metallicity regimes. Excluding stars with mass <0.7
(including those stars will result in even stronger correlations),
linear fits result in slopes of 6, 3, 2, 2 dex
for
stars in the metallicity ranges -1.3 < [Fe/H] < -1.0,
-1.6 < [Fe/H] < -1.3,
-2.5 < [Fe/H] < -1.6,
and -3.5 < [Fe/H] < -2.5. The slopes are
significant at the 8, 2, 5, 1
level, respectively. The correlation coefficient
is 0.9, 0.6, 0.6, 0.3, and the probability of a correlation between
and mass arising by pure chance is very small: 5
10-5, 3
10-2, 1
10-3, and 1.3
10-1,
for stars in the same metallicity ranges as above. Thus, the correlations of
and mass
in different metallicity regimes are very significant.
![]() |
Figure 5:
Li abundances as a function of stellar mass in different metallicity ranges. The metal-poor ([Fe/H] |
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Recently, González Hernández et al. (2008, hereafter G08) have studied the metal-poor ([Fe/H] -3.5)
double-lined spectroscopic binary BPS CS22876-032, providing thus
crucial data to test our Li-mass trend. With our method and the stellar
parameters of G08, we obtain a mass ratio of 0.89, very close to their
value (0.911
0.022) obtained from an orbital solution.
For the primary we obtain MA = 0.776
,
and adopting the mass ratio of G08, MB = 0.707
is obtained for the secondary. The LTE Li abundances were taken from
G08 and corrected for NLTE effects (
-0.05 dex). The components of the binary are shown as circles in Fig. 5, nicely following the trend of the most metal-poor stars. Including this binary
in our sample would strengthen the Li-mass correlation of stars with [Fe/H] < -2.5. A slope =3 dex
significant at the 3
level is obtained, with
= 0.5 and a low probability (2
10-2) of the trend being spurious.
While mass-dependent Li depletion is expected from standard models of
stellar evolution, this should only occur at significantly lower masses
than considered here. These stellar models only predict very minor 7Li depletion ( dex) for metal-poor turn-off stars (e.g. Pinsonneault et al. 1992), which is far from sufficient to explain the
0.5 dex
discrepancy between the observed Li abundance and predictions from
BBN+WMAP. Bridging this gap would thus require invoking stellar models
that include additional processes normally not accounted for,
such as rotationally-induced mixing or diffusion.
In Fig. 5 we confront the predictions of Richard et al. (2005)
with our inferred stellar masses and Li abundances. The models
include the effects of atomic diffusion, radiative acceleration, and
gravitational settling, but moderated by a parameterized turbulent
mixing (T6.0, T6.09, and T6.25, where higher numbers mean higher
turbulence); so far only the predictions for
[Fe/H] = -2.3 are available for different turbulent mixing
models. The agreement is very good when adopting a turbulent model of
T6.25 (see Richard et al., for the meaning of this notation)
and an initial
;
had the Kurucz convective overshooting models been adopted, the
required initial abundance to explain our observational data would
correspond to
.
Two other weaker turbulence models that produce smaller overall Li depletions are also shown in Fig. 5,
but they are less successful in reproducing the observed
Li abundance pattern. Our best-fitting turbulence
model (T6.25) is different from that (T6.0) required to
explain the abundance pattern in the globular cluster NGC 6397 at
similar metallicity (Korn et al. 2006; Lind et al. 2009b). Another problem with adopting this high turbulence is that the expected corresponding 6Li depletion would amount to >1.6 dex and thus imply an initial 6Li abundance at least as high as the primordial 7Li abundance if the claimed 6Li detections in some halo stars (A06; AM08) are real.
Our results imply that the Li abundances observed in Li plateau stars have been depleted from their original values and therefore do not represent the primordial Li abundance. It appears that the observed Li abundances in metal-poor stars can be reasonably well reconciled with the predictions from standard Big Bang nucleosynthesis (e.g. Cyburt et al. 2008) by means of stellar evolution models that include Li depletion through diffusion and turbulent mixing (Richard et al. 2005). We caution however that although encouraging, our results should not be viewed as proof of the Richard et al. models until the free parameters required for the stellar modelling are better understood from physical principles.
AcknowledgementsWe thank the referee for valuable comments to strengthen the presentation of our results. We thank J. R. Shi for providing the EW measurements used in S07, O. Richard for providing tables with the Li depletion models, R. Collet, P. Nissen, A. García Peréz, D. Fabbian and L. Sbordone for providing data to estimate E(B-V) from interstellar Na I D lines, K.Lind for providing NLTE abundance corrections in electronic form. This work has been partially supported by FCT (project PTDC/CTE-AST/65971/2006, and Ciencia 2007 program).
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Online Material
Table 1: Parameters and Li abundances of our metal-poor stars.
Footnotes
- ... depletion
- Based in part on observations obtained at the W. M. Keck Observatory, the Nordic Optical Telescope on La Palma, and on data from the HIRES/Keck archive and the European Southern Observatory ESO/ST-ECF Science Archive Facility.
- ...
- Table 1 is only available in electronic form at http://www.aanda.org
- ...
K
- In some cases the
given in Table 1 may be slightly different from the
given in C10 due to improved input parameters (e.g., better E(B-V) values) in the IRFM used here. The conclusions of C10 are unaffected by these minor changes.
- ...
-1
- The adopted relation between
[
/Fe] and [Fe/H] ignores the detailed abundance patterns of the two discs and halos (e.g., Ramírez et al. 2007; Nissen & Schuster 2010).
- ... stars
- Except for the work of B05, who provide comparisons at different metallicities but for cool severely Li-depleted dwarfs, i.e. probably of lower mass than most stars shown in Fig. 5
All Tables
Table 1: Parameters and Li abundances of our metal-poor stars.
All Figures
![]() |
Figure 1: Adopted E(B-V) values vs. [Fe/H]. Filled squares are values based on NaD lines and open squares on reddening maps. |
Open with DEXTER | |
In the text |
![]() |
Figure 2:
Li abundances vs.
|
Open with DEXTER | |
In the text |
![]() |
Figure 3:
Li abundances for stars with
|
Open with DEXTER | |
In the text |
![]() |
Figure 4:
a) Filled circles show the slope/ |
Open with DEXTER | |
In the text |
![]() |
Figure 5:
Li abundances as a function of stellar mass in different metallicity ranges. The metal-poor ([Fe/H] |
Open with DEXTER | |
In the text |
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