Results 341 to 350 of about 114,517 (388)
Photon strength functions and nuclear level densities: invaluable input for nucleosynthesis. [PDF]
Philos Trans A Math Phys Eng SciWiedeking M, Goriely S.
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Optimizing photosynthetic light-harvesting under stars: Generalized thermodynamic models
Chitnavis S +6 more
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The crystallization of white dwarf stars [PDF]
Nature Astronomy, 2019 Recent observations with the Gaia satellite have confirmed that the cores of cooling white dwarf stars undergo crystallization, as predicted half a century ago.
M Hugh, Van Horn
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Buoyant crystals halt the cooling of white dwarf stars.
NatureWhite dwarfs are stellar remnants devoid of a nuclear energy source, gradually cooling over billions of years1,2 and eventually freezing into a solid state from the inside out3,4.
A. Bédard, S. Blouin, Sihao Cheng
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, 1992 White dwarf stars represent the most common endpoint of stellar evolution. In fact, about 90% of all stars will end up as white dwarfs. Their high temperatures and low luminosities imply that they are small — only about the size of the Earth (R e = 0.009R⊙). The mean radius for white dwarfs is R = 0.01 R⊙ (see the first table).
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Annual Review of Astronomy and Astrophysics, 1980
The violated rule to which Professor Eddington referred was the mass luminosity relation for dwarf stars. The "strange objects" had the exceed ingly low luminosities of the faint red dwarfs, yet their colors were quite bluish. Thus, they came to be called white dwarfs.
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The violated rule to which Professor Eddington referred was the mass luminosity relation for dwarf stars. The "strange objects" had the exceed ingly low luminosities of the faint red dwarfs, yet their colors were quite bluish. Thus, they came to be called white dwarfs.
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Physics of white dwarf stars [PDF]
Reports on Progress in Physics, 1990 White dwarf stars, compact objects with extremely high interior densities, are the most common end product in the evolution of stars. The authors review the history of their discovery, and of the realisation that their structure is determined by the physics of the degenerate electron gas.
Detlev Koester, G. Chanmugam
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