Abstract
view Abstract Citations (11) References (38) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Thermal pulses in helium shell-burning stars. Faulkner, D. J. ; Wood, P. R. Abstract The helium shell-burning evolution of a 0.8 star has been calculated with a detailed treatment of the abundance profile in the shell source. Contrary to a suggestion by Paczyn.ski that pure helium stars are thermally stable when so treated, the star undergoes a single thermal pulse before entering the white-dwarf region at the end of its evolution. Since Kutter has found a 1.04 star to be stable, 0.8 appears to be the upper mass limit for the thermal instability phenomenon in pure helium stars. The decay time of the thermal pulse is in good agreement with the observed rate of evolution for the nuclei of planetary nebulae, and it is suggested that planetary-nebula shells may be ejected by radiation pressure during such a pulse. The calculations show that further pulse events are possible even if the shell ejection removes all hydrogen-rich material. The present pulse was not sufficiently luminous, however, to eject any helium-rich material. Publication: The Astrophysical Journal Pub Date: November 1972 DOI: 10.1086/151781 Bibcode: 1972ApJ...178..207F full text sources ADS | data products SIMBAD (1)
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