neutron star 中文意思是什麼

neutron star 解釋
【天文學】中子星。

  • neutron : n. 【物理學】中子。n. -ics 中子（物理）學。
  • star : n 1 星；【天文學】恆星 （opp planet）。2 星狀物，星（形勛）章。3 【印刷】星形號〈 〉。4 【占星術...
  1. The model comprising accretion onto a neutron star or black hole companion must still be considered a favored hypothesis.

    在中子星或黑洞伴星上發生吸積的模型，仍應看成是一個有價值的假說。
  2. In the april 14 physical review letters, investigators at the university of basel in switzerland and their colleagues suggest antineutrinos streaming in huge numbers from the neutron star could irradiate the protons and turn some into neutrons, which build stable, heavy isotopes

    在4月14日的《物理評論通訊》中，瑞士巴塞爾大學的研究人員與合作伴提出，從中子星大量湧出的反微中子會照射質子，並使部份質子轉變為中子，以形成穩定的重同位素。
  3. There has been many papers to discuss the in - medium quark and gluon condensates in nuclear matter which use the models with su ( 2 ) l su ( 2 ) r sym - metry. now, we make use of the chiral model su ( 3 ) l su ( 3 ) n including the baryon octet to discuss the quark condensate < qq > in strange matter, where q is an up or down quark field. on the one hand, from the experimetal data, it is found that < qq > vac = - ( 225 25mev ) 3, on the other hand, with the hellmann - feynman theorem, quark condensate can be evaluated on the hadronic level. in this paper, we will investigate the quark condensate in strange matter with the chiral symmetry su ( 3 ) l x su ( 3 ) rspontaneous breaking lagrangian to obtain the variation of the quark condensate in the strange matter when the baryon number change. it can be applied to understand the neutron stars when the neutron star are considered to be constructed by the strange matter. because nertron stars are homogeneous and at very low temperature, we will use the mean - field approximation and zero temperature throughout this paper

    鑒于已有大量文獻討論了核物質中的夸克凝聚，本文將討論在奇異物質中的夸克凝聚。而在介質中的夸克凝聚的基本公式可由hellmann - feynman理論導出，所以運用手征對稱自發破缺拉氏量以及平均場近似，我們就可以討論在奇異物質中的夸克凝聚，由所計算的結果表明： （ 1 ）奇異物質中的夸克凝聚隨奇異物質密度的增大而單調減小。 （ 2 ） -凝聚的出現對衰減率有影響。
  4. Does a neutron star represent the ultimate in compression ?

    中子星是壓縮的最終產物嗎？
  5. In the first seconds after a supernova, a region rich in protons emerges around the dead star ' s core, which has most likely collapsed into a neutron star

    在發生超新星爆炸后的最初幾秒內，這個死亡恆星的核心（最可能塌縮形成中子星的地方）周圍，會產生一個富含質子的區域。
  6. For example, if there is a planet orbiting around the neutron star, it will wobble a little and the pulses will come a little early or late. we can then deduce the mass and the radius of the orbit of the planet from the arrival time of the pulses. this is how the first extrasolar planet is discovered

    例如假若有一顆行星圍繞一顆中子星運行，它會令中子星出現搖動，引致脈沖的間隔變長或短，由此我們根據脈沖周期的變化，可推斷出行星的質量和軌道半徑，這亦是天文學家找出第一顆地外行星時所用的方法。
  7. A quantitative analysis of this idea led to the prediction that a star remaining about three times the mass of the sun at the end of its evolution ( usually as a neutron star ), will almost inevitably shrink to the critical size needed to undergo a gravitational collapse

    該想法的定量分析導致預言一顆恆星在終止它演化時候保持大約三倍太陽的質量（通常看做一顆中子星） ，將會幾乎不可避免收縮到臨界體積必須遭受引力坍塌。
  8. The strong gravitational field of a neutron star provides the answer

    中子星的超強引力提供了最佳的解答。
  9. The results show that - condensate appears at some baryon densities and makes great effect to the curve of state equation of neutron star ; hyperons - and a exist in neutron star matter at high desities

    結果表明， ~ -凝聚將出現在一定的重子密度區間，並對中子星狀態方程曲線有重要的影響；超子~ -和在較高密度也會出現。
  10. In this model, the resulting implosion and ensuing explosion would blow off the outer envelope of the star and leave behind the core as a neutron star.

    按此模型，引起的突然壓縮和隨后的爆發會把恆量的外部包層吹跑，留下的核成為一顆中子星。
  11. Finally, due to the rapid rotation of the neutron star, or the evolution of the companion, the infall of matter stops, the x - ray emission declines, and the neutron star emerges as a radio - emitting millisecond pulsar

    最後，由於中子星疾速的自轉，或是伴星自身的演化，物質的流入停止， x射線輻射減弱，這顆中子星就呈現出了毫秒脈沖星的面目。
  12. When electrons move in spirals around magnetic lines of force, radio waves are produced and radiated out along the two magnetic poles of the star. usually, the rotational axis of the neutron star does not align with the magnetic axis. the radiation beams will sweep around and create the

    通常恆星的自轉軸和磁軸並不一致，中子星亦不例外，所以沿著磁軸向外發射的無線電波束，在中子星自轉的帶動下，便會如燈塔般向宇宙掃射，這便是著名的
  13. Structure of a pulsar ? a rotating magnetic neutron star

    脈沖星的結構。一顆旋轉磁中子星。
  14. Such high speed was considered unusual for a neutron star

    這麼高的速度對中子星來說是很不尋常的。
  15. 1 neutron star is a star that is largely made up of neutrons

    中子星是一顆大部份物質為中子的星球。
  16. If the moving fluid in a newborn neutron star also transfers a tenth of its kinetic energy to the magnetic field, then the field would grow stronger than 1015 gauss, which is more than 1, 000 times as strong as the fields of most radio pulsars

    如果在新生中子星里的流體，也把10 %的動能轉變成磁場的話，磁場強度會上漲到超過1015高斯，這是大多數無線電波霎所帶磁場強度的1000倍以上。
  17. Since a 7 - solar - mass is too large to be a white dwarf or neutron star, it must be a black hole

    因為有著7個太陽質量的星體不可能是白矮星或中於星，所以它一定是黑洞。
  18. Can stop the star from further collapsing. note : again, neutron degenerate pressure does not come from nuclear burning. it can support a neutron star from further gravitational contraction forever

    則足以防止恆星進一步收縮同電子簡並壓力一樣中子簡並壓力並非來自核子反應它可永遠?抗恆星的引力收縮。
  19. Since the gravitational field on the surface is very strong, no hills or mountains can be formed on a neutron star

    由於引力場實在太強大，任何山脈高山皆會被引力蕩平，所以中子星的表面十分光滑。
  20. By analogy, a neutron star born rotating as fast as or faster than the convective period of 10 milliseconds could develop a widespread, ultrastrong magnetic field

    以此類推，在中子星誕生的時候，要是它的自轉速率和10毫秒的對流周期一樣快，甚至更快，就能發展出大區域的超強磁場。
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