Minimum stellar mass

The evolution of a 17.5 M0 star, chosen to be similar to the precursor of SN1987A, has been studied using the input physics described in Wood and Faulkner (1987). The calculations use opacities from the Astrophysical Opacity Library of Huebner et al (1977) with H, He, C, N, O and other metals in LMC ratios treat semi-convection in the manner of Lamb, Iben and Howard (1976) and assume the mass loss rate to be the minimum of (a) a times the rate give in Waldron (1985) (this rate applied in the blue part of the HR diagram), and (b) L/(cv) (this rate applied in the red), where v is the stellar wind expansion velocity which was taken to be 12 km s 1. 

Turbulent mixing and dust disk evolution models for a range of stellar and disk masses correlations are much easier to observe and more difficult to fit than simulations restricted to the minimum-mass solar nebula... 

Figure 9.3 Mass accretion rates versus the age of the stellar group. The age error bars represent typical uncertainties, while die accretion rate error bars are the maximum and minimum values measured in each region. In addition to the data presented in Calvet et al. (2005), we have included the mass accretion rates from p Ophiuchi (Natta et al. 2006), and from a Orionis (Gatti et al. 2008). Above the plot we show a comparison to the formation timescale of CAIs, chondrules, and the moon lapetus in the Solar System (see Sections 9.3.1 and 9.3.2).

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