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  2. I Zwicky 18 - Wikipedia

    en.wikipedia.org/wiki/I_Zwicky_18

    I Zwicky 18 is thus unlikely to have formed all its stars recently in a cold dark matter Universe. [5] [6] Later observations with the Hubble Space Telescope found faint and old stars contained within the galaxy, suggesting its star formation started at least one billion years ago and possibly as much as ten billion years ago. The galaxy ...

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  4. NGC 602 - Wikipedia

    en.wikipedia.org/wiki/NGC_602

    NGC 602c is a looser grouping 11 arc-minutes to the NE, which includes the WO star AB8. [9] NGC 602 includes many young O and B stars and young stellar objects, with few evolved stars. [10] Ionisation in the nebula is dominated by Sk 183, an extremely hot O3 main sequence star visible as the bright isolated star at the centre of the Hubble ...

  5. Carina–Sagittarius Arm - Wikipedia

    en.wikipedia.org/wiki/Carina–Sagittarius_Arm

    The Carina–Sagittarius Arm is one of the most pronounced arms in our galaxy as many HII regions, young stars and giant molecular clouds are concentrated in it. [ 2 ] The Milky Way is a barred spiral galaxy , consisting of a central crossbar and bulge from which two major and several minor spiral arms radiate outwards.

  6. NASA discovers the 'loneliest' star in the universe - AOL

    www.aol.com/news/2016-07-28-nasa-discovers-the...

    In a galaxy far, far away from any known celestial object, a young star is going through a tremendous yet incredibly lonely growth spurt -- much like you did in middle school.

  7. Spiral galaxy - Wikipedia

    en.wikipedia.org/wiki/Spiral_galaxy

    Spiral arms appear visually brighter because they contain both young stars and more massive and luminous stars than the rest of the galaxy. As massive stars evolve far more quickly, [30] their demise tends to leave a darker background of fainter stars immediately behind the density waves. This make the density waves much more prominent.

  8. Hubble sequence - Wikipedia

    en.wikipedia.org/wiki/Hubble_sequence

    Hubble defined two classes of irregular galaxy: [16] Irr I galaxies have asymmetric profiles and lack a central bulge or obvious spiral structure; instead they contain many individual clusters of young stars; Irr II galaxies have smoother, asymmetric appearances and are not clearly resolved into individual stars or stellar clusters

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