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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 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 [5] [6] First singular white dwarf with a planet WD 1145+017: 2015 WD 1145+017 b: Planet is extremely small and is disintegrating. First white dwarf that is a pulsar: AR Scorpii A ...

  4. Category:Stars by luminosity class - Wikipedia

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

    Download as PDF; Printable version; ... White dwarfs. Red dwarfs. Subdwarfs. Main sequence ... Pages in category "Stars by luminosity class"

  5. 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 ...

  6. 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 .

  7. 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]

  8. Main sequence - Wikipedia

    en.wikipedia.org/wiki/Main_sequence

    The common use of "dwarf" to mean the main sequence is confusing in another way because there are dwarf stars that are not main-sequence stars. For example, a white dwarf is the dead core left over after a star has shed its outer layers, and is much smaller than a main-sequence star, roughly the size of Earth. These represent the final ...

  9. White dwarf - Wikipedia

    en.wikipedia.org/wiki/White_dwarf

    White dwarf - Wikipedia