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  2. AR Aurigae - Wikipedia

    en.wikipedia.org/wiki/AR_Aurigae

    As the name implies, these stars have over-abundances of the elements mercury and manganese, and also often xenon and other elements. [4] Because AR Aurigae is an eclipsing binary (in fact, it is the only known eclipsing binary with a mercury-manganese star), accurate characterization of its parameters has been made possible.

  3. 64 Aurigae - Wikipedia

    en.wikipedia.org/wiki/64_Aurigae

    64 Aurigae is a single [7] star located 312 [1] light years away from the Sun in the northern constellation of Auriga. [6] It is visible to the naked eye as a dim, white-hued star with an apparent magnitude of 5.87. [2]

  4. Iota Aurigae - Wikipedia

    en.wikipedia.org/wiki/Iota_Aurigae

    Iota Aurigae (ι Aurigae, abbreviated Iota Aur, ι Aur), officially named Hassaleh / ˈ h æ s É™ l eɪ /, [12] is a star in the northern constellation of Auriga.It has an apparent visual magnitude of 2.7, [2] which is bright enough to be readily visible to the naked eye.

  5. AB Aurigae - Wikipedia

    en.wikipedia.org/wiki/AB_Aurigae

    AB Aurigae is a young Herbig Ae star [3] in the Auriga constellation. It is located at a distance of approximately 509 light years from the Sun based on stellar parallax. [1] This pre-main-sequence star has a stellar classification of A0Ve, [4] matching an A-type main-sequence star with emission lines in the spectrum.

  6. AE Aurigae - Wikipedia

    en.wikipedia.org/wiki/AE_Aurigae

    It is approximately 1,300 light-years from Earth. AE Aur is a runaway star that might have been ejected during a collision of two binary star groups. This collision, which also is credited with ejecting Mu Columbae and possibly 53 Arietis , has been traced to the Trapezium cluster in the Orion Nebula two million years ago.

  7. R Aurigae - Wikipedia

    en.wikipedia.org/wiki/R_Aurigae

    R Aurigae (R Aur) is a Mira variable, a pulsating red giant star in the constellation of Auriga, at a distance of 930 light years. In 1862 R Aurigae was found to be a variable star at Bonn Observatory. [9] It was widely observed in the late 19th century and its spectrum was described in 1890. [10]

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