main-sequence lifetime

The main-sequence lifetime (MS lifetime) of a star is largely determined by its mass, with metallicity also taking a role, per the Vogt-Russell theorem. Rotation also has a role and interaction with a binary companion can take a substantial role in cases where it occurs. The typical lifetime with no such interaction varies from millions of years for the most massive stars, to trillions for those with barely enough mass for hydrogen burning. (The more-massive star has the shorter lifetime: it has more fuel, but this is more than compensated for by its higher rate of fuel-consumption due to its higher central density and temperature.) A star's MS time occupies a large majority of its total lifetime leading up to its becoming a stellar remnant. A very rough estimate of a star's main-sequence lifetime based upon its mass is:

τ = 1010 (MSun/M)2.5

• τ - a star's main-sequence lifetime.
• M_Sun - mass of the Sun.
• M - mass of the star.