Entretien avec Jean Charbonnel

Charbonnel, Jean; Dulphy, Anne; Manigand, Christine

doi:10.3917/hp.017.0179

Cited by 1 publication

(3 citation statements)

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“…Some researches (e.g. Brown et al 1989, Charbonnel & Balachandran 2000, Ramírez et al 2012 show that the previous results indicate the fraction of Li-rich giants is less than 1%, which agrees well with our results. To check the mass and evolutionary status of the Li-rich and Li-normal giants, we plot their positions in H-R diagram in Figure 7, by adopting the stellar evolutionary tracks of YY (Yi et al 2003) with the mean metallicity Z = 0.008 ([Fe/H] = -0.4, blue line) and solar metallicity Z = 0.02 ([Fe/H] = 0, green line).…”

Section: Li-rich Stars and Li-normal Starssupporting

confidence: 93%

“…As a result of selection strategy in our sample, i.e., only late G and K giants are selected for planet search program, the majority of stars which are classified as RGBs are located in the same region of the H-R diagram. According to the statement of Charbonnel & Balachandran(2000), the Li production phase is very short, which supports the result of observations that less than 1% giants are Li-rich, as confirmed both in previous studies and our work.…”

Section: Li-rich Stars and Li-normal Starssupporting

confidence: 93%

“…The mixing result in the production of 7 Li, which is then convected to the surface. We know that 96% of the evolved stars show a low 12 C/ 13 C ratio (Charbonnel & Do Nascimento 1998), which is in disagreement with standard predictions. Thus the most reasonable explanation is that they have undergone a period of Li-production.…”

Section: Li-rich Stars and Li-normal Starscontrasting

confidence: 66%

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The Lithium Abundances of a Large Sample of Red Giants

Liu

Tan

Wang

et al. 2014

ApJ

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The lithium abundances for 378 G/K giants are derived with non-LTE correction considered. Among these, there are 23 stars that host planetary systems. The lithium abundance is investigated, as a function of metallicity, effective temperature, and rotational velocity, as well as the impact of a giant planet on G/K giants. The results show that the lithium abundance is a function of metallicity and effective temperature. The lithium abundance has no correlation with rotational velocity at vsini < 10 km s −1 . Giants with planets present lower lithium abundance and slow rotational velocity (vsini < 4 km s −1 ). Our sample includes three Li-rich G/K giants, 36 Li-normal stars and 339 Li-depleted stars. The fraction of Li-rich stars in this sample agrees with the general rate of less than 1% in literature, and the stars that show normal amounts of Li are supposed to possess the same abundance at the current interstellar medium. For the Lidepleted giants, Li deficiency may have already taken place at the main sequence stage for many intermediate-mass (1.5-5 M ⊙ ) G/K giants. Finally, we present the lithium abundance and kinematic parameters for an enlarged sample of 565 giants using a compilation of literature, and confirm that the lithium abundance is a function of metallicity and effective temperature. With the enlarged sample, we investigate the differences between the lithium abundance in thin-/thick-disk giants, which indicate that the lithium abundance in thick-disk giants is more depleted than that in thin-disk giants.

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Section: Li-rich Stars and Li-normal Starssupporting

confidence: 93%

Section: Li-rich Stars and Li-normal Starssupporting

confidence: 93%

Section: Li-rich Stars and Li-normal Starscontrasting

confidence: 66%

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