Abstract
Theoretical prediction of surface stellar abundances of light elements–lithium, beryllium, and boron–represents one of the most interesting open problems in astrophysics. As well known, several measurements of 7Li abundances in stellar atmospheres point out a disagreement between predictions and observations in different stellar evolutionary phases, rising doubts about the capability of present stellar models to precisely reproduce stellar envelope characteristics. The problem takes different aspects in the various evolutionary phases; the present analysis is restricted to protostellar and pre-Main Sequence phases. Light elements are burned at relatively low temperatures (T from ≈2 to ≈5 million degrees) and thus in the early evolutionary stages of a star they are gradually destroyed at different depths of stellar interior mainly by (p, α) burning reactions, in dependence on the stellar mass. Their surface abundances are strongly influenced by the nuclear cross sections, as well as by the extension toward the stellar interior of the convective envelope and by the temperature at its bottom, which depend on the characteristics of the star (mass and chemical composition) as well as on the energy transport in the convective stellar envelope. In recent years, a great effort has been made to improve the precision of light element burning cross sections. However, theoretical predictions surface light element abundance are challenging because they are also influenced by the uncertainties in the input physics adopted in the calculations as well as the efficiency of several standard and non-standard physical processes active in young stars (i.e. diffusion, radiative levitation, magnetic fields, rotation). Moreover, it is still not completely clear how much the previous protostellar evolution affects the pre-Main Sequence characteristics and thus the light element depletion. This paper presents the state-of-the-art of theoretical predictions for protostars and pre-Main Sequence stars and their light element surface abundances, discussing the role of (p, α) nuclear reaction rates and other input physics on the stellar evolution and on the temporal evolution of the predicted surface abundances.
Highlights
Light elements – lithium, beryllium and boron – are burned at relatively low temperatures (T from ≈ 2 to ≈ 5 million degrees) easy to reach in stellar interiors at the bottom of the convective envelope, even during the early preMain Sequence evolution
The predicted depletion of surface lithium abundance is affected by the uncertainties on the input physics adopted in stellar models and on the assumed chemical composition, that influence the extension of convective envelope and temperature structure of the star
Pre-Main Sequence (MS) characteristics and surface light element abundances depend on the previous protostellar phase, which is the phase when the star forms
Summary
Light elements – lithium, beryllium and boron (hereafter Li, Be and B) – are burned at relatively low temperatures (T from ≈ 2 to ≈ 5 million degrees) easy to reach in stellar interiors at the bottom of the convective envelope, even during the early preMain Sequence (pre-MS) evolution. The pre-MS is the first stellar phase where the star evolves as a fully formed object To reach this evolutionary stage, the future star has to accrete mass, until its final value, in the previous “protostellar phase.”. The present review summarizes the state-of-the-art of theoretical predictions for protostars and pre-MS stars and their light element surface abundances, in the light of recent improvements in the adopted input physics, updated reaction rates and description of the formation and evolution of preMS stars.
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