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1.A sudden change in the period of rotation of a neutron star.
中子星旋转周期的突然变化收藏指正
2.Structure of a pulsar — a rotating magnetic neutron star.
脉冲星的结构。一颗旋转磁中子星收藏指正
3.One-Dimensional Accretion Column Model ofa Magnetized Neutron Star
中子星的一维吸积柱模型收藏指正
4.Neutron superfluid vertex in neutron stars is discussed in this paper.
摘要讨论了中子星内中子超流涡旋。收藏指正
5.The Spontaneous Broken Symmetry and Acoustic Speed in The Neutron Stars
中子星中的对称性自发破缺与声速收藏指正
6.Effect of f_0(975) and φ(1020) Mesons on Neutron Star Mater
f_0(975)和Φ(1020)介子对中子星物质的影响收藏指正
7.ABNORMAL NEUTRON STAR WITH ABNORMAL PROTONS II. INHOMOGENEOUS STELLAR MODEL
含有反常质子的反常中子星II.非均匀星体模型收藏指正
8.Once the mass is found, it can be determined if the candidate is a neutron star or a black hole.
一旦获得了质量,就可以判断这个候选体是中子星还是黑洞。收藏指正
9.Astronomers knew several examples of neutron stars that lie within supernova remnants.
天文学家早就知道好些个位在不同超新星残骸里的中子星收藏指正
10.Using the RMF theory to describe the neutron liquid region in the neutron star and the Fermi gas model or FMT, BPS, and BBP model to describe the crust of the neutron star (referred as Fermi gas+RMF and RMF* respectively), the properties of the neutron star are calculated and compared with those from the RMF theory.
利用相对论平均场理论描述中子星的液体区域,Fermi气体模型或者FMT,BPS和BBP模型描述中子星外壳,分别称为Fermigas+RMF和RMF . 计算了中子星性质并且和相对论平均场理论给出的结果进行比较.收藏指正
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