Fusion Reaction of ^16O＋^14N and Its Implication for the Production of ^26Al in Explosive Oxygen Burning

We suggest that the fusion reaction ^16O＋^14N may be a new way to produce ^26Al in interstellar medium. Adopting different mixing modes, we investigate the impact on the production of ^26Al in explosive oxygen burning and find that the result is extremely sensitive to mixing mechanisms. In some cases, we obtain an encouraging result, for example, the greatest final abundance of ^26Al reaches 7.779×10^-6, which means that the explosive oxygen burning may be a new origin of ^26 Al.     

Pulsar Spin—Down by ^3P2 superfluid Neutron with Field Decay

To describe pulsar spin-down,we present a simple combined torque model that takes into account both the standard magnetic dipole radiation and the electromagnetic radiation from the 3P2 superluid vortex neutrons inside neutron star.Using an ordinary exponential model for the magnetic field decay,we derive an analytical formulae for pulsar evolution tracks,The pulsar evolution on the P-P diagram is quite different from that of the standard magnetic dipole radiation model,especially when the superfluid torque or field decay becomes dominant.     

A Hybrid Spin—Down Model and its Application to the Radio Quiet X—Ray Pulsar 1E 1207.4—5209

A series of newly published papers are focusing on the formation of the absorption features discovered by Chandra and XMM-Newton from the young radio quiet x-ray pulsar 1E 1207.4-5209.We try to interpret it as cyclotron absorption lines since this possibility could not be ruled out .With new development and application of a hybrid model.i.e.,the magnetic dipole spin-down model combined with the neutrino cyclotron radiation spin-down model.we can easily avoid the contradiction between the normal rotation energy loss rate and the relatively lower magnetic field,and then we obtain the possible initial spin period(-0.420s) .We suppose that the progenitor of 1E 1207.4-5209 may be a white dwarf.     

Neutrino Lensing

Due to the intrinsic properties of neutrinos, the gravitational lens effect for a neutrino should be more colorful and meaningful than the normal lens effect of a photon. Other than the experiments operated at terrestrial laboratory, in principle, we can propose a completely new astrophysical method to determine not only the nature of the gravity of lens objects but also the mixing parameters of neutrinos by analyzing neutrino trajectories near the central objects. However, the angular, energy and time resolution of the neutrino telescopes are still comparatively poor, so we just concentrate on the two classical tests of general relativity, i.e. the angular deflection and the time delay of the neutrino by a lens object as a preparative work in this paper. In addition, some simple properties of neutrino lensing are investigated.     

The Renormalized Equation of State and Quark Star

By means of the EOS of QCD at zero temperature and finite quark chemical potential we proposed [Phys. Rev. D 78 （2008） 054001] in the framework of rainbow-ladder approximation of Dyson-Schwinger approach, we investigate the structure of quark star and its property. It is found that the mass-radius relation in our model is very different from that of usual quark star models, but similar to neutron star models. The obtained mass of quark star is about 1.75M⊙- 2.2M⊙. The obtained radius of quark star is 22 - 26 km, which is obviously larger than the results in other models. The reason for this discrepancy is analyzed.     

Cosmic Neutrino Oscillation or Separation

Current experiment results show that neutrinos have non-zero masses and that different neutrino flavours may mix and undergo a transformation to each other. Neglecting matter effects for simplicity and by solving the Friedmann-Robertson-Walker geodesic equations of the time-like particle, we preparatively investigate the vacuum oscillation or separation of neutrinos on the cosmic scale.     

旋转荷电球体外部引力场中引力效应

以实验粒子的短程线方程为出发点，计算了由旋转参量与电荷参量所引起的近日点进动效应．当粒子绕行方向与场源旋转方向一致时，与Kerr场中情况相比修正项将使进动效应增大．此外，通过引入局域洛伦兹空间截面，可给出该场中运动物体上加速度．显然在随动系中（vⁱ=0），从极轴方向和赤平面粒子均不能到达场源，而是分别停滞在r＝k＋(k²+4m²a²)^1/2/2m和r=k/m处．此时可以计算对星系尘埃的吸积作用，即尘埃的分布状况．最后还讨论了赤平面上作圆周运动物体（仅v³≠0）的类柯里奥利加速度 关键词：     

A Possible Mechanism for the Origin of Ultrastrong Magnetic Field of Magnetars

Growing observations reveal that soft gamma-ray repeaters and anomalous x-ray pulsars are magnetars. Their magnetic fields may achieve 10^14 - 10^15G. We explore the origin of the superstrong magnetic field by considering the magnetization of the ^3P2 superfluid neutrons inside neutron stars （NSs）. By solving the Tolman-Oppenheimer-Volkov equations together with the equation of state adopted by Elgaroy it et al. [Phys. Rev. Lett. 77 （1996） 1428] in the calculation of the neutron pairing gap, we specifically calculate the NS internal structure, the permissible region for ^3P2 superfluid neutrons inside the NS, and the total magnetic moment contributed by the orderly arranged neutron vortexes. The result shows that the induced magnetic field may cover a wide range, which is consistent with the magnetic field predicted by the standard magnetic dipole radiation for pulsar spindown.