Low-mass red giants and masses of NPNs

Details Low-mass red giants and masses of NPNs Low-mass red giants and masses of NPNs

Mar 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992ap%26ss.189...11h&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 189, no. 1, March 1992, p. 11-21.

Astronomy and Astrophysics

Astrophysics

4

Planetary Nebulae, Red Giant Stars, Stellar Evolution, Stellar Mass, Stellar Mass Ejection, White Dwarf Stars, Asymptotic Giant Branch Stars, Hertzsprung-Russell Diagram, Stellar Models

Scientific paper

The evolutionary track of low-mass red giant stars (0.7-0.9 solar mass) is computed with the aim to demonstrate the conditions under which low-mass white dwarfs (WDs) can form through the evolution of single stars. Also, the influence of the mixing length to the scale height ratio on the radius of the star is calculated, and the coupling between the mixing-length and the mass-loss rate parameters is investigated. The conclusions are that the uncertainties in mass-loss and mixing-length to scale-height ratio leave enough parameter space to allow the formation of low-mass WD via single star evolution. It is concluded that the gap between proto-WD stars without any nebula and stars with well-defined nebulae is bridged by stars which have a dilute gas cloud around them which cannot be observed as a nebula.

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