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中子星
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  neutron star
     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
短句来源
     Hyperon rms Radii of _Λ~(208)Pb and Neutron Star Structure
     _Λ~(208)Pb的超子分布半径和中子星结构
短句来源
     Theoretical Analysis of X-ray Cyclotron Absorption Lines for the Isolated Neutron Star 1E1207.4-5209
     对孤立中子星1E1207.4—5209 X-射线回旋吸收线的理论分析
短句来源
     The maximum mass of the neutron star is calculated to be 1.3~1.4M_⊙.
     由计算结果得中子星的最大质量为1.3~1.4M⊙(M⊙为太阳质量),与观测结果基本相符.
短句来源
     Calculation yields the maximum mass, radius, moment of inertia and central mass density of a neutron star under such a condition are 2,37 m, 11.1 km, 4.3×1045 gcm2 and 2.23×1015 gem-3 respectively.
     所得到的中子星最大质量及相应的星体半径、转动惯量和中心密度分别为:2.37M_⊙,11.1km,4.3×10~(45)gcm~2和2.32×10~(15)gcm~(-3)。
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  neutron stars
     The Oppenheimer-Volkoff mass limits of neutron stars calculated from different equations of state are 1.52—2.06 M_(⊙), and the radii are 10.24—11.38 km with hyperons included.
     对于中子星, 考虑超子后不同参数组给出的质量极限的范围为 1. 52—2. 06M⊙,半径为 10. 24—11. 38km.
短句来源
     The electron capture of the nuclide 56Co and 59Fe,as the examples,are investigated in a strong magnetic field at the crusts of Neutron stars.
     以核素56Co和59Fe为例,讨论了强磁场中子星外壳层电子俘获.
短句来源
     Direct URCA Process in Neutron Stars
     中子星的直接URCA过程
     The results show that the magnetic field has only a slight effect on the electron capture rates at the range of the magnetic fields(104—1014 T) on surfaces of the most neutron stars.
     结果表明,绝大部分中子星表面的磁场范围104~109T,磁场对电子俘获率的影响很小.
短句来源
     A new exact solution of slow rotation structure equation of rotating perfect fluid spheres on neutron stars
     中子星的理想流体球模型的慢旋转结构方程的新精确解
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  “中子星”译为未确定词的双语例句
     Two satisfactory Skyrme interactions, SKM and SG2, give rise to a maximum masses with M max =1.7 M ⊙, M max =1.67 M ⊙.
     对于SKM和SG2这两个较好的Skyrme相互作用模型计算得到中子星的最大质量分别为Mmax=1 .7M⊙ ,Mmax=1 .67M⊙ .
短句来源
     The maximum masses calculated from different EOS are 2.0—3.0M ⊙, and the corresponding radius are 10—14km.
     相应的中子星的最大质量也不同 ,不同有效相互作用给出的最大质量为 2 .0— 3.0M⊙ ,从大到小的顺序依次是NLSH ,NL3,NL1,DD ME1,TW 99,TM1和GL 97,对应的半径为 10— 14km .
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     We study the influence of the strong interactions between quarks on observational effects of strange stars.
     奇异星是类似于中子星的由奇异夸克物质组成的致密天体。 本文研究了夸克之间的强作用对奇异星观测效应的影响。
短句来源
     The authors also import two other kinds of three body forces, AV14+TBF and Paris+TBF, into their calculations for a comparison.
     为便于比较 ,文中还计算了AV1 4+TBF和Paris+TBF这两种三体相互作用模型下的中子星的性质
短句来源
     According to this theory,the formula of photon wavelength in synchrotron radiation is found out, and the calculation results of wavelength is consonant with experimental data.
     给出了同步辐射实光子的波长的计算公式,并从合肥国家同步实验室和北京同步辐射装置的峰值特征波长以及斯坦福直线加速器中心的Ec/E3e 值、强磁场中子星极区的同步辐射等方面验证了该公式的正确性。
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  neutron star
This conclusion is consistent with the model of a circumstellar envelope but is inconsistent with the existence of an accretion disk around the neutron star.
      
Energy release during disk accretion onto a rapidly rotating neutron star
      
Based on the static criterion for stability, we present a method of constructing the dependence of gravitational mass M on Kerr rotation parameter j and on total baryon mass (rest mass) m for a rigidly rotating neutron star.
      
Energy release on the surface of a rapidly rotating neutron star during disk accretion: A thermodynamic approach
      
Expressions are derived for the energy release during accretion onto a cool (with constant entropy), rapidly rotating neutron star (NS) in the Newtonian theory and in general relativity.
      
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  neutron stars
This velocity closely corresponds to a pulsar escape velocity of ≈1000 km s-1 (at a total mass of ≈1.9M⊙ for the binary of neutron stars).
      
During the observations, 47 X-ray bursts were detected, 33 of which are most likely type I bursts related to unstable helium burning on the surfaces of neutron stars.
      
New generation mechanisms for X-ray quasi-periodic oscillations in accreting neutron stars
      
The photon-cavitation mechanism is considered when studying X-ray QPOs in neutron stars with critical (Eddington) luminosities.
      
A model of low-mass neutron stars with a quark core
      
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The emission mechanism from X-ray soturces in close binary stars is studied.It is suggested that pair production may play an important role in the X-ray emission region which is formed by the accretion of a compact object(a neutron star or a black hole).The present model accounts qualitatively for the following observed general properties in X-ray binaries: 1.The X-ray luminosity lies within the range 10~(36)—10~(38)erg/sec. 2.The X-ray energy spectrum can in the majority of cases be represented either the power-law...

The emission mechanism from X-ray soturces in close binary stars is studied.It is suggested that pair production may play an important role in the X-ray emission region which is formed by the accretion of a compact object(a neutron star or a black hole).The present model accounts qualitatively for the following observed general properties in X-ray binaries: 1.The X-ray luminosity lies within the range 10~(36)—10~(38)erg/sec. 2.The X-ray energy spectrum can in the majority of cases be represented either the power-law or the thermal bremsstrahlung form. 3.The temperature of the thermal bremsstrahlung spectrum is the order of 10~8K. 4.The form of the energy spectrum does not change appreciably when the luminosity fluctuates.

本文研究了密近双星中的 X 射线源的发射机制.本文提出:在致密星(中子星或黑洞)的吸积所形成的 X 射线发射区中,电子对的产生起着重要的作用.这种模型可以定性地说明 X射线双星所具有的几个一般的观测特征,即:1.它们的 X 射线光度都在10~(36)—10~(38)尔格/秒范围中.2.X 射线能谱为幂形式,或热韧致形式.3.热韧致谱的温度数量级为10~K.4.当光度涨落时,能谱形式无明显变化.

Recently, although many authors have calculated the masses of the neutron stars, the yielded upper limits of their masses are yet quite different, as shown in Fig. 1. The curves A-G are yielded with nonrelativistic theories: N and 0, with relativistic ones, and S is the result of our present work. For the purpose of comparison, the results observed by authors P. C. Joss, et al. are shown at the right in Fig. 1. It is obvious that for the high densities (above 2×1014 g/cm3) the calculation of nonrelativistic...

Recently, although many authors have calculated the masses of the neutron stars, the yielded upper limits of their masses are yet quite different, as shown in Fig. 1. The curves A-G are yielded with nonrelativistic theories: N and 0, with relativistic ones, and S is the result of our present work. For the purpose of comparison, the results observed by authors P. C. Joss, et al. are shown at the right in Fig. 1. It is obvious that for the high densities (above 2×1014 g/cm3) the calculation of nonrelativistic is not reliable. But Walecka's mean field approach is rather better. He assumed that the neutron star is a system of uniformly distributed nuclei and the interactions between them proceed from the field of the neutral vector meson fields, both the neutral scalar meson. Besides, he assumed that the classical meson fields, both vector and scalar, are constants-independent of the spacetime coordinates. These assumptions are illustrated by the formulas (1) and (7) (8) respectively. The two free parameters (cs2 and cv2) contained in Walecka's model are adjusted to fit the nuclear density and binding energy at saturation (Fermi wave number kF = 1.42fm-1, eeeeeeeeeeeB=-15.75 MeV). A third bulk property of nuclear matter at saturation-impressibility kv-1 obtained by experiment is 220 MeV, while the Walecka's model yields kv-1= 550 MeV. In view of the fact mentioned above, we, on the basis of the Walecka's model, propose some improvements as follows:1. The average interparticle distance of nuclear matter at saturation (about 1 fm) compared with the range (0.25 fm) of ω-meson interaction with nucleon is large, so that this assumption (8) when it is in the neighbourhood of saturation point is not suitable. Then, we propose that in the derivation of the vector meson interaction energy, the uniform nucleon distribution is treated as being not completely independent of spatial position, but rather as lattice points separated by average distance determined from the densities, i.e. replacing (8) with (15). Following the way initiated by Walecka, we obtain the equation of state of dense matter, given by (16) and (17). Fig. 2 and Fig. 3 are the comparisons of the present result, with Walecka's work.2. The constants Cv2, gv and mv contained in (15) and (16) being treated as three free parameters can be adjusted to fit the three experimental data kF, SB and Kv-1.In section 3, we calculate Mmax and I of a neutron star, using our present model and the equations of relativistic stellar structure. The results are Mmax=1.7M⊙ and I= 1.67×1045 g·cm2. It is much nearer the observational data.The comparisons of the present results with Walecka's work are given by Fig. 4 and Fig. 5.We find that the modified mean field model reduces the disagreement between the relativistic and nonrelativistic theories in their predictions of masses and moments of inertia.

我们用改进的平均场方法计算了核密度以上物质的状态方程,并用中子星结构方程计算了中子星结构,得出引力质量M_G=1.7M_⊙,转动惯量I=1.62×10~(45)g-cm~2。结果表明,这些值与观测值符合的较好;高密物质相互作用模型的选取直接影响到中子星结构的特征量,同时可看出,用改进的平均场方法可使非相对论和相对论理论所推算的中子星的质量和转动惯量之间的差距明显地缩小。

In this paper an idea of existing a nutation partition layer (probably a thin layer) in superficial region of the Earth is introduced and therefore a new nutation model is advanced. Equations of polar motion based on it and a more universal solution are given. It is proved that partition layer is in the nature of "soft", locates at depth of about 300 km. Its viscosity is about 1010 poises, similar to that of pitch at 15℃ and allowable minimum thickness is possibly less than 1 km. Conclusions are given as following:...

In this paper an idea of existing a nutation partition layer (probably a thin layer) in superficial region of the Earth is introduced and therefore a new nutation model is advanced. Equations of polar motion based on it and a more universal solution are given. It is proved that partition layer is in the nature of "soft", locates at depth of about 300 km. Its viscosity is about 1010 poises, similar to that of pitch at 15℃ and allowable minimum thickness is possibly less than 1 km. Conclusions are given as following: "Chandler frequency" is double, of which one is the frequency of nutation of outer part and other is that of inner of the Earth. The period of " 40" years in amplitude is only a beat of these two frequencies. The ratio in amplitude of two terms responding to these frequencies is about10" 125/0." 175=0.7. The empirical relation between the amplitude and period of C.W. is a direct result of this theory. Abrupt change of arc of polar motion and sudden 180° phase change are substantially different parts of same phenomenon. Both of them depond on relative changes of nutation frequencies of inner and outer part. Value of Q(30-60) determined before is a pseudo-Q. Real value of Q for C.W. is nearly 200, which is in agreement to that from seismic waves. It is predicted that in addition to two main frequencies there is a series of secondary frequencies distributing symmetrically about either of these two main C.W. frequencies, that the raw pole should mainly move to and from along or across the mean trace owing to continuous excitations and exchanges of energies of two parts and that the time constant of C. W. is about 70 and it can nearly be maintained by earthquake excitations.

本文引进了在地球上表层存在一个章动隔离层的概念,从而建立了一种新的章动模型,求出了运动方程及其解。在天体物理中,中子星的自转与章动问题与此类似,本文也许能供研究此类问题时参考。业已证明,地球的隔离层的性质是“软”的,大约位于地表以下300公里的深度。允许的最小厚度小于1公里,它的粘滞率大约为10~(10)泊的量级,相当于沥青在15℃时的情况。结果表明,钱德勒摆动的“主峰”是双频,其一是内主体的章动频率,另一是外体本身的章动频率。由于两个频率的拍频作用而产生钱德勒振幅的40年变化周期。两项的振幅互相影响,因而大小相差不大,它们的近似比值是0.7。著名的钱德勒摆动的振幅-周期关系是本文的直接结果。地极运动弧形的急变与1924—1926年左右的180°相变在本质上是一回事,它们是由内、外体的章动频率的相对变化决定的。过去人们从观测中定出的钱德勒摆动Q值在30—60之间,这是一个假Q值,真正的Q值是200左右,和由地震波定出的Q值一致。本文的解还预言,除两个主频率外,其两旁还对称地分布着一系列(一对以上)次要频率。钱德勒摆动的时间常数约为70年,它近似可由地震激发所维持。它的非平滑运动将主要沿平均迹线方向...

本文引进了在地球上表层存在一个章动隔离层的概念,从而建立了一种新的章动模型,求出了运动方程及其解。在天体物理中,中子星的自转与章动问题与此类似,本文也许能供研究此类问题时参考。业已证明,地球的隔离层的性质是“软”的,大约位于地表以下300公里的深度。允许的最小厚度小于1公里,它的粘滞率大约为10~(10)泊的量级,相当于沥青在15℃时的情况。结果表明,钱德勒摆动的“主峰”是双频,其一是内主体的章动频率,另一是外体本身的章动频率。由于两个频率的拍频作用而产生钱德勒振幅的40年变化周期。两项的振幅互相影响,因而大小相差不大,它们的近似比值是0.7。著名的钱德勒摆动的振幅-周期关系是本文的直接结果。地极运动弧形的急变与1924—1926年左右的180°相变在本质上是一回事,它们是由内、外体的章动频率的相对变化决定的。过去人们从观测中定出的钱德勒摆动Q值在30—60之间,这是一个假Q值,真正的Q值是200左右,和由地震波定出的Q值一致。本文的解还预言,除两个主频率外,其两旁还对称地分布着一系列(一对以上)次要频率。钱德勒摆动的时间常数约为70年,它近似可由地震激发所维持。它的非平滑运动将主要沿平均迹线方向来回运动。

 
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