Main-sequence mass loss and the lithium dip

Details Main-sequence mass loss and the lithium dip Main-sequence mass loss and the lithium dip

Aug 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...359l..55s&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 359, Aug. 20, 1990, p. L55-L58.

Astronomy and Astrophysics

Astrophysics

55

Lithium, Main Sequence Stars, Stellar Evolution, Stellar Mass Ejection, Abundance, Beryllium, Stellar Mass, Stellar Oscillations

Scientific paper

The significant dip in observed lithium abundances for Population I stars near M about 1.3 solar mass is discussed. It is noted that this dip occurs near where the instability strip crosses the main sequence on the lower edge of the Delta Scuti stars and that stellar pulsations are expected to give rise to mass loss. A total mass loss of 0.05 solar mass over the main-sequence lifetime of these stars would be sufficient to explain the observations of lithium depletion. The absence of a dip in the Pleiades and of significant depletion of beryllium in the Hyades places tight constraints on the rate of mass loss. These constraints make unlikely the high main-sequence mass-loss rates which would significantly affect globular cluster ages.

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