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  2. 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]

  3. SDSS 1557 - Wikipedia

    en.wikipedia.org/wiki/SDSS_1557

    SDSS 1557 (SDSS J155720.77+091624.6, WD 1554+094) is a binary system composed of a white dwarf and a brown dwarf.The system is surrounded by a circumbinary debris disk.The debris disk was formed when a minor planet was tidally disrupted around the white dwarf in the past.

  4. WD J0651+2844 - Wikipedia

    en.wikipedia.org/wiki/WD_J0651+2844

    WD J0651+2844 is a white dwarf binary star system composed of two white dwarfs. [2] They are approximately 120,000 km apart and complete an orbit around their barycenter in less than 13 minutes. [1] This produces an eclipse every 6 minutes. This makes it possible to gather enough data to produce extremely accurate predictions of each future ...

  5. List of neutron stars - Wikipedia

    en.wikipedia.org/wiki/List_of_Neutron_stars

    They are created as a result of supernovas and gravitational collapse ... Binary with a white dwarf PSR J1719−1438 ... High-mass X-ray binaries; Centaurus X-3 ...

  6. Laser Interferometer Space Antenna - Wikipedia

    en.wikipedia.org/wiki/Laser_Interferometer_Space...

    One of the currently known binaries that LISA will be able to resolve is the white dwarf binary ZTF J1539+5027 with a period of 6.91 minutes, the second shortest period binary white dwarf pair discovered to date. [47] [48]

  7. White dwarf - Wikipedia

    en.wikipedia.org/wiki/White_dwarf

    Sirius B, which is a white dwarf, can be seen as a faint point of light to the lower left of the much brighter Sirius A. A white dwarf is a stellar core remnant composed mostly of electron-degenerate matter. A white dwarf is very dense: its mass is comparable to the Sun's and its volume Earth's.

  8. Symbiotic binary - Wikipedia

    en.wikipedia.org/wiki/Symbiotic_binary

    They usually contain a white dwarf with a companion red giant. The cool giant star loses material via Roche lobe overflow or through its stellar wind, which flows onto the hot compact star, usually via an accretion disk. Symbiotic binaries are of particular interest to astronomers as they can be used to learn about stellar evolution.

  9. AM Canum Venaticorum star - Wikipedia

    en.wikipedia.org/wiki/AM_Canum_Venaticorum_star

    AM CVn stars with a white-dwarf donor can be formed when a binary consisting of a white dwarf and a low-mass giant evolve through a common-envelope (CE) phase. The outcome of the CE will be a double white-dwarf binary. Through the emission of gravitational radiation, the binary loses angular momentum, which causes