2L
＋＋＋＋＋＋＋＋＋＋＋＋＋＋＋＋此楼简介＋＋＋＋＋＋＋＋＋＋＋＋＋＋＋＋＋＋＋
FOR ALL MY BELOVED FRIENDS
HERE IS JUST A STORAGE ROOM
FOR SOME TRIVIAL KNOWLEDGE
OR MAYBE
JUST DUE TO MY OWN PERSONAL
INTERESTS.
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#1 昏迷的原理————————摘自度娘
意识障碍的最严重阶段。意识清晰度极度降低，对外界刺激无反应，程度较轻者防御反射及生命体征可以存在，严重者消失。昏迷既可由中枢神经系统病变引起（占70％），又可以是全身性疾病的后果，如急性感染性疾病、内分泌及代谢障碍、心血管疾病、中毒及电击、中暑、高原病等均可引起昏迷。 根据程度分为：①浅昏迷。对强烈痛刺激有反应，基本生理反应存在，生命体征正常。②中度昏迷。对痛刺激的反应消失，生理反应存在，生命体征正常。③深昏迷。除生命体征存在外，其他均消失。④过度昏迷。即脑死亡。 某些部位的病变可出现一些特殊的昏迷：①醒状昏迷。又称去皮质状态。两侧大脑半球广泛性病变。②无动性缄默症。网状结构及上行激活系统病变。③闭锁综合征。桥脑腹侧病变。 昏迷应与嗜睡、意识混浊、昏睡及木僵等鉴别。昏迷时常有生命体征的急剧变化。多种生理参数（心、肺功能、体温、脑电图、肾功能及各种生理反射等）的监测是必不可少的。首要的是针对病因积极治疗，预防合并症，保护心、肺、肾及中枢神经系统功能。 昏迷的定义 昏迷是觉醒状态与意识内容以及躯体运动均完全丧失的一种极严重的意识障碍，对强烈的疼痛刺激也不能觉醒。 昏迷的病因分类 颅内、外疾病昏迷病因分类 Plum学派的昏迷病因分类 Adams的昏迷病因分类 颅内、外疾病昏迷病因分类 颅外疾病（全身性疾病） 1.代谢性脑病 2.中毒性脑病 颅内疾病 1.肿块性或破坏性病变 2.弥漫性病变 代谢性脑病 肝性脑病 肾性脑病 肺性脑病 心脏脑病（心脏停搏、心肌梗死、严重心律紊乱） 胰性脑病 胃肠脑病 糖尿病酸中毒昏迷 非酮性高渗性昏迷 代谢性脑病 低血糖昏迷 内分泌脑病（垂体性昏迷、粘液水肿、甲状腺脑病、肾上腺危象） 缺氧性脑病（窒息、休克脑病、贫血性脑病、高山昏迷、肺栓塞、溺水、自缢、电击） 电解质、酸碱失衡 体温失衡（中暑、低温昏迷）

Stellar nucleosynthesis
is the collective term for the nucleosynthesis, or nuclear reactions, taking place in stars to build the nuclei of the elements heavier than hydrogen. Some small quantity of these reactions also occur on the stellar surface under various circumstances. For the creation of elements during the explosion of a star, the term supernova nucleosynthesis is used. The processes involved began to be understood early in the 20th century, when it was first realized that the energy released from nuclear reactions accounted for the longevity of the Sun as a source of heat and light. The prime energy producer in the sun is the fusion of hydrogen to helium, which occurs at a minimum temperature of 3 million kelvin.

In 1920, Arthur Eddington, on the basis of the precise measurements of atoms by F.W. Aston, was the first to suggest that stars obtained their energy from nuclear fusion of hydrogen to form helium. In 1928, George Gamow derived what is now called the Gamow factor, a quantum-mechanical formula that gave the probability of bringing two nuclei sufficiently close for the strong nuclear force to overcome the Coulomb barrier. The Gamow factor was used in the decade that followed by Atkinson and Houtermans and later by Gamow himself and Edward Teller to derive the rate at which nuclear reactions would proceed at the high temperatures believed to exist in stellar interiors. In 1939, in a paper entitled "Energy Production in Stars", Hans Bethe analyzed the different possibilities for reactions by which hydrogen is fused into helium. He selected two processes that he believed to be the sources of energy in stars. The first one, the proton-proton chain, is the dominant energy source in stars with masses up to about the mass of the Sun. The second process, the carbon-nitrogen-oxygen cycle, which was also considered by Carl Friedrich von Weizsäcker in 1938, is most important in more massive stars. These works concerned the energy generation capable of keeping stars hot. They did not address the creation of heavier nuclei, however. That theory was begun by Fred Hoyle in 1946 with his argument that a collection of very hot nuclei would assemble into iron.[1] Hoyle followed that in 1954 with a large paper outlining how advanced fusion stages within stars would synthesize elements between carbon and iron in mass. Quickly, many important omissions in Hoyle's theory were corrected, beginning with the publication of a celebrated review paper in 1957 by Burbidge, Burbidge, Fowler and Hoyle (commonly referred to as the B2FH paper).[2] This latter work collected and refined earlier research into a heavily cited picture that gave promise of accounting for the observed relative abundances of the elements. Significant improvements were made by A. G. W. Cameron and by Donald D. Clayton. Cameron presented his own independent approach (following Hoyle) of nucleosynthesis. He introduced computers into time-dependent calculations of evolution of nuclear systems. Clayton calculated the first time-dependent models of the S-process, the R-process, the burning of silicon into iron-group elements, and discovered radiogenic chronologies for determining the age of the elements. The entire research field expanded rapidly in the 1970s.

The most important reactions in stellar nucleosynthesis:
Hydrogen burning:
Deuterium burning
The proton-proton chain
The carbon-nitrogen-oxygen cycle
Helium burning:
The triple-alpha process
The alpha process
Burning of heavier elements:
Carbon burning process
Neon burning process
Oxygen burning process
Silicon burning process
Production of elements heavier than iron:
Neutron capture:
The R-process
The S-process
Proton capture:
The Rp-process
Photo-disintegration:
The P-process


虽然看不懂但好像lz很厉害的样子。
十五字十五字十五字十五字十五字十五字！