Sentence examples for stellar life from inspiring English sources

So called because the smaller varieties almost resemble planetary disks when viewed through a telescope, planetary nebulae represent a stage at the end of the stellar life cycle rather than one at the beginning.

The new details may also help scientists better understand the other end of the stellar life cycle: star birth.

Dust grains are formed at the end of the stellar life, in the stellar wind of asymptotic giant branch stars (e.g., Ferrarotti and Gail, 2006), in the stellar ejecta of supernovae (e.g., Nozawa et al., 2003; Rho et al., 2008), among others.

Memphis, Tennessee-born and Oberlin College-educated Mary Church Terrell (1863 1954) lived a stellar life of articulate leadership in uplift and advocacy organizations devoted to the development and well-being of Colored women (Colored Women's League, the National Association of Colored Women), commitments articulated in "The Progress of Colored Women" (1898, published 1904) and other writings.

In about 5 billion years, the sun will grow when it becomes a red giant, devouring Mercury and Venus as it nears the end of its stellar life.

Unlike the Sun, massive stars possess the mass needed to fuse elements that have an atomic mass greater than hydrogen and helium, albeit at increasingly higher temperatures and pressures, causing increasingly shorter stellar life spans.

Most stars (including the sun) go through a variable stage, so they are used to study stellar life-cycles, among other things.

The stellar life-time τ1f(m) is calculated by the formula of Raiteri et al. (1996) which is a fitting function of Padova stellar evolutionary tracks (Bertelli et al., 1994).

The mass-returned rate from dying stars, R, is given by (8 where (9)is the time at which stars with mass m dying at time t are born, τ1f(m) is the stellar life-time, w(m, Z) is the remnant mass of stars with mass m and metallicity Z, and m1f (t) is the minimum mass of stars dying at time t.

Here, let us adopt the instantaneous recycling approximation (IRA) in which we neglect the finite stellar life-time and assume that stars with a mass larger than a certain threshold (the turn-off mass mt) die instantly when they are formed.

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