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In astrophysics, Chandrasekhar's white dwarf equation is an initial value ordinary differential equation introduced by the Indian American astrophysicist Subrahmanyan Chandrasekhar, [1] in his study of the gravitational potential of completely degenerate white dwarf stars.
These stars are intermediate in size between red M-type main-sequence stars ("red dwarfs") and yellow/white G-type main-sequence stars. They have masses between 0.6 and 0.9 times the mass of the Sun and surface temperatures between 3,900 and 5,300 K . [ 1 ]
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 ...
A light year is the distance light travels in a year, 5.9 trillion miles (9.5 trillion km). Janus is fairly massive for a white dwarf, with a mass 20% larger than that of our sun compressed into ...
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: in an Earth sized volume, it packs a mass that is comparable to the Sun.
The Chandrasekhar limit (/ ˌ tʃ ə n d r ə ˈ ʃ eɪ k ər /) [1] is the maximum mass of a stable white dwarf star.The currently accepted value of the Chandrasekhar limit is about 1.4 M ☉ (2.765 × 10 30 kg).
What exactly is a white dwarf star, you ask? NASA explains, "As stars like our sun age, they puff up into red giants and then gradually lose about half their mass, shrinking down to 1/100th of ...
The white dwarf star completes a full rotation once every 25 seconds. Skip to main content. Sign in. Mail. 24/7 Help. For premium support please call: 800-290-4726 ...