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  2. White dwarf - Wikipedia

    en.wikipedia.org/wiki/White_dwarf

    While old white dwarfs show evidence of dust accretion, white dwarfs older than ~1 billion years or >7000 K with dusty infrared excess were not detected [175] until the discovery of LSPM J0207+3331 in 2018, which has a cooling age of ~3 billion years. The white dwarf shows two dusty components that are being explained with two rings with ...

  3. WD J0914+1914 - Wikipedia

    en.wikipedia.org/wiki/WD_J0914+1914

    The team was also able to exclude accretion of material from a companion star or brown dwarf. [4] The most plausible explanation is an evaporating giant planet, orbiting close to the white dwarf. The atmosphere of the planet is evaporated by the strong ultraviolet radiation of the hot white dwarf. The planet is likely to be about 15 solar radii ...

  4. Cataclysmic variable star - Wikipedia

    en.wikipedia.org/wiki/Cataclysmic_variable_star

    Some result from white dwarfs in binary systems but others are very massive stars. (Classical) novae: These cataclysmic variables have very large outbursts, of 6 to 19 magnitudes, caused by thermonuclear fusion of material accreted onto the white dwarf. Recurrent novae These have outbursts of about 4 to 9 magnitudes, repeating every 10 to 80 ...

  5. Radiation-induced cancer - Wikipedia

    en.wikipedia.org/wiki/Radiation-induced_cancer

    Radiation hormesis is the conjecture that a low level of ionizing radiation (i.e., near the level of Earth's natural background radiation) helps "immunize" cells against DNA damage from other causes (such as free radicals or larger doses of ionizing radiation), and decreases the risk of cancer. The theory proposes that such low levels activate ...

  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. G 29-38 - Wikipedia

    en.wikipedia.org/wiki/G_29-38

    Like other young, hot white dwarfs, G29-38 is thought to have formed relatively recently (600 million years ago) from its AGB progenitor, and therefore the excess was naturally explained by emission from a Jupiter-like brown dwarf with a temperature of 1200 K and a radius of 0.15 solar radius.

  8. WD 0032−317 - Wikipedia

    en.wikipedia.org/wiki/WD_0032%E2%88%92317

    The white dwarf WD 0032−317 is located about 1,400 light years from Earth. [1] WD 0032−317 formed about three billion years ago when a low mass star (possibly of 1.3 solar masses) expanded into its red giant phase. The star then blew out its outer layers leaving behind the helium-rich core (which is WD 0032−317).

  9. van Maanen 2 - Wikipedia

    en.wikipedia.org/wiki/Van_Maanen_2

    Like other white dwarfs, it is a very dense star: its mass has been estimated to be about 67% of the Sun's, [28] yet it has only 1% of the Sun's radius (1.23 times the Earth's radius) [8] [a] The outer atmosphere has a temperature of approximately 6,110 K, [28] which is relatively cool for a white dwarf. As all white dwarfs steadily radiate ...