Mass-luminosity relation

With the assumptions of Section 11.3.2, and assuming a mass-luminosity relation L oc Ml s, show that the Fundamental Plane satisfies the relations... 

For WR stars less luminous than 3 105 (i.e. Mwr 20 Mq) no strict mass-luminosity relation exists. 

The luminosity of HD 50896 was determined to log (L/L ) =5.3 (model A), or less in the case of a smaller distance (cf. Table 1). A complrison with recent evolutionary calculations by Maeder and Meynet (1987) indicates an actual mass of about 10 M (case A) from the (extrapolated) mass-luminosity relation for WR stars. Bu unfortunately, stars of this luminosity do not become WR stars, according to these evolutionary models, since the corresponding tracks (e.g. for an initial mass of 20 M ) never return to the blue side of the HR diagram. 

Hertzsprung-Russell, Mass-Luminosity Relations, and Binary Stars... 

The IMF is derived locally from the present day mass function (PDMF) which in turn is obtained by counting the Main Sequence stars per interval of magnitude. Then the star counts are transformed into number of stars per pc2 and then a mass-luminosity relation is adopted to pass from the luminosity to the mass. 

The mass-luminosity relation averaged over the whole main sequence (Sect. 2.3) is empirically... 

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