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  2. Hertzsprung–Russell diagram - Wikipedia

    en.wikipedia.org/wiki/Hertzsprung–Russell_diagram

    Eddington predicted that dwarf stars remain in an essentially static position on the main sequence for most of their lives. In the 1930s and 1940s, with an understanding of hydrogen fusion, came an evidence-backed theory of evolution to red giants following which were speculated cases of explosion and implosion of the remnants to white dwarfs.

  3. List of white dwarfs - Wikipedia

    en.wikipedia.org/wiki/List_of_white_dwarfs

    First solitary white dwarf Van Maanen 2: 1917 Van Maanen's star is also the nearest solitary white dwarf [5] First white dwarf with a planet WD B1620−26: 2003 PSR B1620-26 b (planet) This planet is a circumbinary planet, which circles both stars in the PSR B1620-26 system [6] [7] First singular white dwarf with a transiting object WD 1145+017 ...

  4. Dwarf star - Wikipedia

    en.wikipedia.org/wiki/Dwarf_star

    The Hertzsprung–Russell diagram showing the location of main sequence dwarf stars and white dwarfs. A dwarf star is a star of relatively small size and low luminosity. Most main sequence stars are dwarf stars. The meaning of the word "dwarf" was later extended to some star-sized objects that are not stars, and compact stellar remnants that ...

  5. Luminosity function (astronomy) - Wikipedia

    en.wikipedia.org/wiki/Luminosity_function...

    The white dwarf luminosity function (WDLF) gives the number of white dwarf stars with a given luminosity. As this is determined by the rates at which these stars form and cool, it is of interest for the information it gives about the physics of white dwarf cooling and the age and history of the Galaxy. [3] [4]

  6. Category:Stars by luminosity class - Wikipedia

    en.wikipedia.org/wiki/Category:Stars_by...

    Print/export Download as PDF; ... White dwarfs. Red dwarfs. Subdwarfs. Main sequence ... Pages in category "Stars by luminosity class"

  7. BPM 37093 - Wikipedia

    en.wikipedia.org/wiki/BPM_37093

    BPM 37093 (V886 Centauri) is a variable white dwarf star of the DAV, or ZZ Ceti, type, with a hydrogen atmosphere and an unusually high mass of approximately 1.1 times the Sun's. It is 48 light-years (15 parsecs ) from Earth in the constellation Centaurus and vibrates; these pulsations cause its luminosity to vary .

  8. White dwarf - Wikipedia

    en.wikipedia.org/wiki/White_dwarf

    White dwarf effective surface temperatures extend from over 150 000 K [24] to barely under 4000 K. [68] [69] In accordance with the Stefan–Boltzmann law, luminosity increases with increasing surface temperature (proportional to T 4); this surface temperature range corresponds to a luminosity from over 100 times that of the Sun to under 1 ...

  9. Category:White dwarfs - Wikipedia

    en.wikipedia.org/wiki/Category:White_dwarfs

    Print/export Download as PDF; Printable version; ... White dwarf star stubs (24 P) Pages in category "White dwarfs"