The Mechanism of the Mass-loss of Stellar Wind for Intermediate-mass Stars

Astronomy and Astrophysics – Astronomy

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Stars: Evolution, Stars: Mass-Loss, Turbulence

Scientific paper

Simultaneously considering the effects of the restriction of the gravitation, the perturbation from the radiation pressure and the turbulence pressure, and the promotion from the convective region in the outer shell of a star by introducing the compressible fluid mechanism, a new formula of the mass-loss of stellar wind is built up in this paper. The stars with initial masses in the range of 3≤ M/M_{&sun;} ≤ 5 have evolved from the main-sequence phase to the end of asymptotic giant branch (AGB). The mass-loss rates with the new formula are in excellent agreement with those with the classical mass-loss formula from the main-sequence phase to the stage of the end of the central helium burning. However, the fluctuation of mass-loss rate with the classical formula has arisen at the end of AGB because of the effect of the surface luminosity. On the contrary, the continuous major mass-loss has been obtained with the new formula at the end of AGB. It is concluded that the mass-loss derived with the new formula is comparatively consistent with the observational results.

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