The relation between initial and minimum final white dwarf mass for Population I stars

Details The relation between initial and minimum final white dwarf mass for Population I stars The relation between initial and minimum final white dwarf mass for Population I stars

Dec 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...311..762m&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 311, Dec. 15, 1986, p. 762-773.

Astronomy and Astrophysics

Astrophysics

38

Stellar Evolution, Stellar Mass Ejection, White Dwarf Stars, Asymptotic Giant Branch Stars, Giant Stars, Main Sequence Stars, Stellar Composition, Stellar Interiors

Scientific paper

The evolutionary paths for Population I stars having initial masses 1, 2.5, 3, 4, and 5 solar masses were computed from the homogeneous main sequence to the onset of the first major thermal pulse to evaluate the minimum mass and the chemical stratification of the remnant white dwarf (WD) associated with each parent mass. The helium flash phase was followed in detail for a 2.5 solar masses star, whereas for the 1 solar mass star the flash was bypassed, and the models at the beginning of the steady central helium burning phase were obtained by means of a scaling procedure upon the properly computed total and core masses. The results show that for a parent ranging between 1-3 solar masses the core mass at the first thermal pulse ranges only from 0.64-0.69 solar mass. If some very fast mass-loss mechanism is triggered in connection with the early stages of the thermal pulse phase, as suggested by the observed deficiency of asymptotic giant branch stars, the relation between final and initial mass is almost flat at least up to an initial mass of 3 solar masses, and the mass spectrum of the WDs is narrow and heavily peaked around 0.65 solar mass.

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