What's A Degenerate
The triakis tetrahedron is a degenerate case with 12 zero-length edges. (In terms of the colors used above this means, that the white vertices and green edges are absorbed by the green vertices.) (In terms of the colors used above this means, that the white vertices and green edges are absorbed by the green vertices.). What's the difference? The skin on our bodies is one massive organ. In fact – skin is the largest organ in the body. Ironically, it is the part of the body that we pay the least attention to. Aging causes our skin to degenerate in its function. ”Every time The Kiwi Farms gets caught trying to condemn children to a life of drugs, gangs, drinking, rape, incest, verbal abuse, physical abuse, and a number of other horrors, it promises it'll never do so again.”.
A dwarf star is a star of relatively small size and low luminosity. Most main sequence stars are dwarf stars. The term was originally coined in 1906 when the Danish astronomer Ejnar Hertzsprung noticed that the reddest stars—classified as K and M in the Harvard scheme could be divided into two distinct groups. They are either much brighter than the Sun, or much fainter. To distinguish these groups, he called them 'giant' and 'dwarf' stars,[1] the dwarf stars being fainter and the giants being brighter than the Sun. Most stars are currently classified under the Morgan Keenan System using the letters O, B, A, F, G, K, and M, a sequence from the hottest: O type, to the coolest: M type. The scope of the term 'dwarf' was later expanded to include the following:
A version of this article appeared in the issue of Publishers Weekly under the headline: “Degenerate” Books for Discerning Readers. Regress definition, to move backward; go back.
- Dwarf star alone generally refers to any main-sequence star, a star of luminosity class V: main-sequence stars (dwarfs). Example: Achernar (B6Vep)[2]
- Red dwarfs are low-mass main-sequence stars.
- Yellow dwarfs are main-sequence (dwarf) stars with masses comparable to that of the Sun.
- Orange dwarfs are K-type main-sequence stars.
- A blue dwarf is a hypothesized class of very-low-mass stars that increase in temperature as they near the end of their main-sequence lifetime.
- A white dwarf is a star composed of electron-degenerate matter, thought to be the final stage in the evolution of stars not massive enough to collapse into a neutron star or black hole—stars less massive than roughly 9 solar masses.
- A black dwarf is a white dwarf that has cooled sufficiently that it no longer emits any visible light.
- A brown dwarf is a substellar object not massive enough to ever fuse hydrogen into helium, but still massive enough to fuse deuterium—less than about 0.08 solar masses and more than about 13 Jupiter masses.
See also[edit]
What's A Degenerate
References[edit]
- ^Brown, Laurie M.; Pais, Abraham; Pippard, A. B., eds. (1995). Twentieth Century Physics. Bristol; New York: Institute of Physics, American Institute of Physics. p. 1696. ISBN0-7503-0310-7. OCLC33102501.
- ^Nazé, Y. (November 2009). 'Hot stars observed by XMM-Newton. I. The catalog and the properties of OB stars'. Astronomy and Astrophysics. 506 (2): 1055–1064. arXiv:0908.1461. Bibcode:2009A&A...506.1055N. doi:10.1051/0004-6361/200912659. S2CID17317459.