M57, The Ring Nebula

 Imaging Equipment

Exposure Information

 About This Image

M57, the Ring Nebula, is a planetary nebula lying in the constellation Lyra. This expanding shell of fluorescing gas is about one light year across and is expanding at 20 to 30km/s. It subtends an angle of about one arcminute and lies at a distance of about 2300 LY based on a trigonometric parallax measurement of the central star.

Planetary nebulae are formed when Sun-like stars come to the end of their nuclear fusion lives. After exhausting the last of the hydrogen gas supply in their cores, swollen red giant stars cast off their outer layers during short-lived fusion events wherein heavier elements undergo brief, violent fusion reactions. The cast off shells of gas creates these glowing nebulae. The cores of the progenitor stars remain intact as dense, super-hot white dwarf stars with surface temperatures of 50,000 to 120,000K; many times hotter than the Sun's 5800K surface temperature. No nuclear reactions continue to generate heat in the white dwarf stars so they eventually cool. But for a while, the high surface temperatures produce intense ultraviolet radiation causing the cast off gasses to fluoresce. Spectroscopic analysis of the light from these nebulae reveals information about the abundance of gasses that constituted the original stars.

The white dwarf star in M57 is clearly visible in this image, lying at the center of the planetary nebula. Its blue color is a result of its very high surface temperature.

This image spans about 10 by 15 arcminutes of sky. For comparison, the full moon spans about 30 arcminutes.

More information about planetary nebulae can be found at APOD.