Owl Nebula
Planetary nebula in the constellation Ursa Major / From Wikipedia, the free encyclopedia
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The Owl Nebula (also known as Messier 97, M97 or NGC 3587) is a planetary nebula approximately 2,030 light years away in the constellation Ursa Major.[2] Estimated to be about 8,000 years old,[6] it is approximately circular in cross-section with a faint internal structure. It was formed from the outflow of material from the stellar wind of the central star as it evolved along the asymptotic giant branch.[5] The nebula is arranged in three concentric shells, with the outermost shell being about 20–30% larger than the inner shell.[7] The owl-like appearance of the nebula is the result of an inner shell that is not circularly symmetric, but instead forms a barrel-like structure aligned at an angle of 45° to the line of sight.[5]
Emission nebula | |
---|---|
Planetary nebula | |
Observation data: J2000.0 epoch | |
Right ascension | 11h 14m 47.734s[1] |
Declination | +55° 01′ 08.50″[1] |
Distance | 2,030 ly (621 pc)[2] 2,800 ly (870 pc)[3] ly |
Apparent magnitude (V) | 9.9[4] |
Apparent dimensions (V) | 3′.4 × 3′.3 |
Constellation | Ursa Major |
Physical characteristics | |
Radius | 0.91 ly (0.28 pc)[5] ly |
Notable features | Owl-like "eyes" visible through larger telescopes |
Designations | M97, NGC 3587, PN G148.4+57.0 |
See also: Lists of nebulae |
The nebula holds about 0.13 solar masses (M☉) of matter, including hydrogen, helium, nitrogen, oxygen, and sulfur;[5] all with a density of less than 100 particles per cubic centimeter.[7] Its outer radius is around 0.91 ly (0.28 pc) and it is expanding with velocities in the range of 27–39 km/s into the surrounding interstellar medium.[5]
The 14th magnitude central star has passed the turning point in its evolution and is condensing to form a white dwarf.[7][8] It has 55–60% of solar mass, is 41 to 148 times solar luminosity (L☉),[5] and has an effective temperature of 123,000 K.[9] The star has been successfully resolved by the Spitzer Space Telescope as a point source that does not show the infrared excess characteristic of a circumstellar disk.[10]