enow.com Web Search

Search results

  1. Results from the WOW.Com Content Network
  2. List of smallest known stars - Wikipedia

    en.wikipedia.org/wiki/List_of_smallest_known_stars

    White dwarfs are stellar remnants produced when a star with around 8 solar masses or less sheds its outer layers into a planetary nebula. The leftover core becomes the white dwarf. It is thought that white dwarfs cool down over quadrillions of years to produce a black dwarf. [15] Neutron star: RX J0720.4−3125: 0.0000064683 – 0.0000077332

  3. Timeline of white dwarfs, neutron stars, and supernovae

    en.wikipedia.org/wiki/Timeline_of_white_dwarfs...

    1930 – Subrahmanyan Chandrasekhar discovers the white dwarf maximum mass limit. 1933 – Fritz Zwicky and Walter Baade propose the neutron star idea and suggest that supernovae might be created by the collapse of normal stars to neutron stars—they also point out that such events can explain the cosmic ray background.

  4. White dwarf - Wikipedia

    en.wikipedia.org/wiki/White_dwarf

    The highly magnetized white dwarf in the binary system AR Scorpii was identified in 2016 as the first pulsar in which the compact object is a white dwarf instead of a neutron star. [120] A second white dwarf pulsar was discovered in 2023.

  5. Compact object - Wikipedia

    en.wikipedia.org/wiki/Compact_object

    The Crab Nebula is a supernova remnant containing the Crab Pulsar, a neutron star. In certain binary stars containing a white dwarf, mass is transferred from the companion star onto the white dwarf, eventually pushing it over the Chandrasekhar limit. Electrons react with protons to form neutrons and thus no longer supply the necessary pressure ...

  6. Binary pulsar - Wikipedia

    en.wikipedia.org/wiki/Binary_pulsar

    An intermediate-mass binary pulsar (IMBP) is a pulsar-white dwarf binary system with a relatively long spin period of around 10–200 ms consisting of a white dwarf with a relatively high mass of approximately . [7] The spin periods, magnetic field strengths, and orbital eccentricities of IMBPs are significantly larger than those of low mass binary pulsars (LMBPs). [7]

  7. Neutron star - Wikipedia

    en.wikipedia.org/wiki/Neutron_star

    A neutron star is the collapsed core of a massive supergiant star. It results from the supernova explosion of a massive star—combined with gravitational collapse—that compresses the core past white dwarf star density to that of atomic nuclei.

  8. Degenerate matter - Wikipedia

    en.wikipedia.org/wiki/Degenerate_matter

    The result is a star with a diameter on the order of a thousandth that of a white dwarf. The properties of neutron matter set an upper limit to the mass of a neutron star, the Tolman–Oppenheimer–Volkoff limit, which is analogous to the Chandrasekhar limit for white dwarf stars.

  9. Stellar classification - Wikipedia

    en.wikipedia.org/wiki/Stellar_classification

    Sub-dwarf classes have also been used: VI for sub-dwarfs (stars slightly less luminous than the main sequence). Nominal luminosity class VII (and sometimes higher numerals) is now rarely used for white dwarf or "hot sub-dwarf" classes, since the temperature-letters of the main sequence and giant stars no longer apply to white dwarfs.