We also provide formulae which model the subsequent remnant phases of evolution. Section 6 discusses the behaviour of a star as the stellar en-velope becomes small in mass and outlines what happens when the nuclear evolution is terminated. Download a PDF of the paper titled Formation of GW190521 from stellar evolution: the impact of the hydrogen-rich envelope, dredge-up and $^$O rate can lead to theįormation of BHs with masses consistent with the primary component of GW190521. In the following, we rst describe the detailed stellar evolution models (Sect.2) and identify the initial mass range for SAGB stars by calculating the pre-AGB evo-lution phase up to the end of the second dredge-up and possibly C-ignition, using three dierent stellar evolu-tion codes (Sect.3). Here we report on a population of low-mass, Tc-rich S stars previously unaccounted for by stellar evolution models. In recent years, the role played by thermohaline mixing in stellar evolution has been widely explored in connection with low-mass RGB evolution. The progress of a stars life is predestined by its mass, because ultimately the mass determines how much energy the star can produce and how quickly it will do so. of second dredge-up and thermal pulses will be discussed.
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