Light Chemical Elements in Stars: Mysteries and Unsolved Problems
The first eight elements of the periodic table are discussed: H, He, Li, Be, B, C, N, and O. They are referred to as key elements, given their important role in stellar evolution. It is noteworthy that all of them were initially synthesized in the Big Bang. The primordial abundances of these elements calculated using the Standard Model of the Big Bang (SMBB) are presented in this review. The good agreement between the SMBB and observations of the primordial abundances of the isotopes of hydrogen and helium, D, 3He, and 4He, is noted, but there is a difference of ~0.5 dex for lithium (the isotope 7Li) between the SMBB and observations of old stars in the galactic halo that has not yet been explained. The abundances of light elements in stellar atmospheres depends on the initial rotation velocity, so the typical rotation velocities of young Main Sequence (MS) stars are examined. Since the data on the abundances of light elements in stars are very extensive, the main emphasis in this review is on several unsolved problems. The helium abundance He/H in early B-type of the MS stars shows an increment with age; in particular, for the most massive B stars with masses M = 12−19M⦿, He/H increases by more than a factor of two toward the end of the MS. Theoretical models of stars with rotation cannot explain such a large increase in He/H. For early B- and late O-type MS stars that are components of close binary systems, He/H undergoes a sharp jump in the middle of the MS stage that is a mystery for the theory. The anomalous abundance of helium (and lithium) in the atmospheres of chemically peculiar stars (types He-s, He-w, HgMn, Ap, and Am) is explained in terms of the diffusion of atoms in surface layers of the stars, but this hypothesis cannot yet explain all the features of the chemical composition of these stars. The abundances of lithium, beryllium, and boron in FGK-dwarfs manifest a trend with decreasing effective temperature T eff as well as a dip at T eff ~ 6600 K in the Hyades and other old clusters. The two effects are among the unsolved problems. In the case of lithium, there is special interest in FGK-giants and supergiants that are rich in lithium (they have logε(Li)≥ 2). Most of them cannot be explained in terms of the standard theory of stellar evolution, so nonstandard hypotheses are invoked: the recent synthesis of lithium in a star and the engulfment by a star of a giant planet with mass equal to that of Jupiter or greater. An analysis of the abundances of carbon, nitrogen, and oxygen in early B- and late O-stars of the MS indicates that the C II, N II, and O II ions are overionized in their atmospheres. For early B-type MS stars, good agreement is found between observations of the N/O ratio and model calculations for rotating stars. A quantitative explanation of the well-known “nitrogen-oxygen” anticorrelation in FGK-giants and supergiants is found. It reflects the dependence of the anomalies in N and C on the initial rotation velocity V0. The stellar rotation models which yield successful explanations for C, N. and O cannot, however, explain the observed helium enrichment in early B-type MS stars.
KeywordsStars chemical composition stellar rotation stellar evolution
Unable to display preview. Download preview PDF.
- 5.R. J. Cooke, M. Pettini, R. A. Jorgenson, et al., Astrophys. J. 781, id. 31 (2014).Google Scholar
- 11.R. H. Cyburt, B. D. Fields, K. A. Olive, et al., Modern Physics, 88, id. 015004 (2016).Google Scholar
- 13.A. Maeder, Physics, Formation and Evolution of Rotating Stars. Springer, Berlin (2009).Google Scholar
- 15.C. W. Allen, Astrophysical Quantities (3 ed.), Athlone Press, London (1973).Google Scholar
- 26.L. S. Lyubimkov, Chemical Composition of Stars: Method and Results of Analysis, Astroprint, Odessa (1995).Google Scholar
- 33.A. M. Boesgaard, Astron. Soc. Pacific Conf. Ser. 336, 39 (2005).Google Scholar
- 34.A. M. Boesgaard, M. G. Lum, C. P. Deliyannis, et al., Astrophys. J. 830, id. 49 (2016).Google Scholar
- 35.L. S. Lyubimkov, D. L. Lambert, B. M. Kaminsky, et al., Mon. Not. Roy. Astron. Soc. 427, 11 (2012).Google Scholar
- 38.C. Aguilera-Gómez, J. Chanamé, M. H. Pinsonneault, et al., Astrophys. J. 829, id. 127 (2016).Google Scholar
- 42.L. S. Lyubimkov, Astrophysics 59, 472 (2016).Google Scholar