Facts about Dumbbell Nebula

1. 06

   In ultraviolet wavelengths, the Dumbbell Nebula emits intense radiation from ionized oxygen and nitrogen, with oxygen producing the characteristic blue-green glow visible in false-color astronomical images.

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   Within its expanding shells, the Dumbbell Nebula's outer regions display filamentary structures visible in optical wavelengths that extend approximately 8 arcminutes across the sky.

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   Messier 27's distinctive dumbbell shape results from the nebula's bipolar structure, where material ejected from the central star expands preferentially along its rotational axis rather than spherically.

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   Observations with the Hubble Space Telescope reveal that the Dumbbell Nebula's central white dwarf star has a surface temperature exceeding 24,000 Kelvin, making it roughly four times hotter than our Sun's surface.

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   The two lobes of this planetary nebula contain an estimated mass equivalent to half our Sun, composed primarily of hydrogen and helium ejected from its central white dwarf star.

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   Approximately 2,600 light-years from Earth, the Dumbbell Nebula expands at roughly 9.4 kilometers per second and was first cataloged by Charles Messier in 1764.

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