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"That is what a star is," he said, "a mass of gas at equilibrium between gravity's inward pressure and outward pressure from nuclear reactions".
The middle stage of evolution occurs when the density has dropped to the point at which the entire mass of gas is ionized.
Compared with diffuse nebulae (see H II region), planetary nebulae are small objects, having a radius typically of 1 light-year and containing a mass of gas of about 0.3 solar mass.
A mass of gas falling rapidly into a black hole is estimated to give off more than 100 times as much energy as is released by the identical amount of mass through nuclear fusion.
The expansion is proportional to the distance from the central star, consistent with the entire mass of gas having been ejected at one brief period from the star in some sort of instability.
In a star, gravity is pulling the mass of gas inward toward a central point, while pressure is pushing the gas outward, and the two competing forces reach a dynamic détente — "simultaneously stable and unstable," you might say — in the form of a sphere.
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They explode leaving expanding masses of gas and dust behind, which, when color-corrected by astronomers, makes for some very pretty pictures.
The present rate of star formation is about one solar mass per year in the entire Galaxy, which contains something like 2 × 109 solar masses of gas.
But farther out from the center, the winds push away and remove about 800 solar masses of gas each year.
These are fireballs, with masses of gas at the head forming bright new stars and leaving a long stream of young stars in their wake.
It is proposed that non steady-state mass transfer of the gas occurs by two mechanisms: (i) mass transfer of gas in clusters or packets of the smaller particles approaching the large particle; and (ii) gas convection.
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