Abstract
In this paper, screened reaction rates and mean lifetimes are studied for the reactions H 11 (Pβ + v)H 12 and He 32 (He3 2H)He 42 in the light of recent work on screening effects. We have interpreted that the dimensionless parameter Γ can remain constant only when the core starts forming and departs from the hydrostatic equilibrium. It is seen that a Main-Sequence star develops its helium core in a very short time after the hydrostatic equilibrium phase. The stellar longevity depends entirely on the reaction H1 (Pβ + v)H2 at the densities ϱX A=102 g cm−3 and 103 g cm−3. Again, the reaction He3(He3 2H)He4 plays a vital role at ϱX A=102 g cm−3 to retain a star for some million years in its Main-Sequence stage.
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Khairozzaman, A.E.M. Screened reaction rates and mean lifetimes for the production of helium in stars. Astrophys Space Sci 107, 233–240 (1984). https://doi.org/10.1007/BF00653529
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DOI: https://doi.org/10.1007/BF00653529