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The computed $\log(\tau/{\rm y})$-$\log(m/m_\odot)$ relation for the stellarinitial mass range, 0.6-120.0, and the stellar initial metallicity range,0.0004-0.0500, tabulated in an earlier attempt (Portinari et al. 1998) isfitted to a good extent by a four-parameter curve, expressed by a doublepower-law, for assigned stellar initial metallicity, which can be reduced to athree-parameter curve, expressed by a single power-law, for the whole set ofstellar initial metallicities. The relative errors do not exceed about 2% and4%, respectively. The extent to which the interpolation curve, expressed by asingle power-law, can be extrapolated towards both high-mass and low-massstars, is also investigated. High-mass star lifetimes are understimated by afactor less than 2 up to $m/m_\odot= 1000$ and by a fiducial factor less than 4up to infinite. Low-mass star lifetimes are overstimated by a factor of about 3down to $m/m_\odot=0.25$ and by an unacceptably large factor down to$m/m_\odot=0.08$. As a simple application, the star mass fraction of a singlestar generation with stellar initial mass function defined by a power-law, isplotted vs. the logarithmic stellar lifetime. The star mass fraction declinesin time at a decreasing rate for mild stellar initial mass function and at anincreasing rate for steep stellar initial mass function, where a linear trendis exhibited for a value of the exponent close to the Salpeter's value, equalto -2.35.

A double power-law fit to the computed stellar $\log(\tau/{\rm y})$-$\log(m/m_\odot)$ relation