Cooling Curve of Strange Star in Strong Magnetic Field

在这篇论文，第一，我们在强壮的磁场从夸克 Urca 过程调查中微子放射率。然后，我们在强壮的磁场讨论奇怪的星的热能力。最后，我们在强壮的磁场给冷却曲线。以便做比较，我们也在空磁场的情况中给相应冷却曲线。没有磁场，结果奇怪的星比那在强壮的磁场更快冷却。

Influence of strong magnetic field on β decay in the crusts of neutron stars

β decay in the strong magnetic field of the crusts of neutron stars is analysed by an improved method. The reactions ^67Ni（β-）^67Cu and ^62Mn（β-）^62Fe are investigated as examples. The results show that a weak magnetic field has little effect on β decay but a strong magnetic field （B 〉 10^12G） increases β decay rates obviously. The conclusion derived may be crucial to the research of late evolution of neutron stars and nucleosynthesis in r-process.

Effect of strong magnetic field on electron capture of iron group nuclei in crusts of neutron stars

In this paper electron capture on iron group nuclei in crusts of neutron stars in a strong magnetic field is investigated. The results show that the magnetic fields have only a slight effect on electron capture rates in a range of 10^5 - 10^13g on surfaces of most neutron stars, whereas for some magnetars the magnetic fields range from 10^13 to 10^18 G. The electron capture rates of most iron group nuclei are greatly decreased, reduced by even four orders of magnitude due to the strong magnetic field.

Structure of Rotating Neutron Stars in Uniform Strong Magnetic Field

在一致强壮的磁场的旋转中子星的性质和变丑是计算的。磁场将弄软中子星物质的状态的方程并且在旋转中子星的结构上做明显的效果。如果磁场是超级的强壮(B = 10 ~(17 ) T ) ，团，半径，和变丑将有效地变得更小。

Effect of Strong Magnetic Field on Gamow-Teller Transition Electron Capture of Iron Group Nuclei at Crusts of Neutron Stars

铁组原子核上的 Gamow 出纳转变的电子俘获在中子星的外壳在一个强壮的磁场被调查。结果证明磁场与磁场的范围在电子俘获率上有仅仅细微效果( 10 9~ 10 13 G )在大多数中子星的表面上，而为某磁铁磁场变化的艺术是 10 13~ 10 18 G ，大多数铁组原子核的电子俘获率将极大地被降低并且可以甚至被减少溢出由强壮的磁场的 3 个数量级。

Effect of superstrong magnetic fields on thermonuclear reaction rates on the surface of magnetars

A simple and efficient screening model for studying the effects of superstrong magnetic fields （such as those of magnetars） on thermonuclear reaction rates on magnetar surfaces is proposed in this paper. The most interesting thermonuclear reactions, including hydrogen burning by the CNO cycle and helium burning by the triple alpha reaction, are investigated on the surface ofmagnetars. We find that the superstrong magnetic fields can increase the thermonuclear reaction rates by many orders of magnitude. The enhancement may have a dramatic effect on the thermonuclear runaways and bursts on the surfaces of magnetars.

Strange Quark Matter and Strangelets in a Strong Magnetic Field

We study the stability properties of magnetized strange quark matter and strangelets under a strong magnetic field in the MIT bag model. The free energy per baryon of strange quark matter feels a great influence from the magnetic field. At the field strength about 1017 G, the magnetized strange quark matter becomes more stable.Considering the finite size effect, the magnetic influence on strangelets becomes complicated. For a given magnetic field, there exists a critical baryon number, below which the magnetized strangelets have lower energy than the nonmagnetized strangelets. For the field strength of 5 × 1017 G, the critical baryon number is Ac～ 100. Generally, the critical baryon number increases with the decreasing external magnetic field. When the field strength is smaller than1017 G, the critical baryon number goes up to Ac～ 105. The stable radius, electric charge, and quark flavor fractions of magnetized strangelets are shown.

Novel quantum phenomena induced by strong magnetic fields in heavy-ion collisions

The relativistic heavy-ion collisions create both hot quark–gluon matter and strong magnetic fields, and provide an arena to study the interplay between quantum chromodynamics and quantum electrodynamics. In recent years, it has been shown that such an interplay can generate a number of interesting quantum phenomena in hadronic and quark–gluon matter. In this short review, we first discuss some properties of the magnetic fields in heavy-ion collisions and then give an overview of the magnetic fieldinduced novel quantum effects. In particular, we focus on the magnetic effect on the heavy flavor mesons, the heavyquark transports, and the phenomena closely related to chiral anomaly.

Bulk viscosity of interacting magnetized strange quark matter

The bulk viscosity of interacting strange quark matter in a strong external magnetic field B m with a real equation of state is investigated.It is found that interquark interactions can significantly increase the bulk viscosity,and the magnetic field B_(m) can cause irregular oscillations in both components of the bulk viscosity,ξ||(parallel to B_(m))and ξ⊥(perpendicular to B_(m)).A comparison with non-interacting strange quark matter reveals that when B_(m) is sufficiently large,ξ⊥is more affected by interactions than ξ||.Additionally,the quasi-oscillation of the bulk viscosity with changes in density may facilitate the for-mation of magnetic domains.Moreover,the resulting r-mode instability windows are in good agreement with observational data for compact stars in low-mass X-ray binaries.Specifically,the r-mode instability window for interacting strange quark matter in high magnetic fields has a minimum rotation frequency exceeding 1050 Hz,which may explain the observed very high spin frequency of a pulsar with V=1122 Hz.

Strange quark mass(ms)dependent model of anisotropic strange quark star

This article presents the configuration of strange quark stars in hydrostatic equilibrium considering the Vaidya-Tikekar metric ansatz.The interior of such stars comprises strange quark matter(henceforth SQM),whose equation of state(hencefor orth EoS)is described by the MIT EoS p=1/3(p-4B),where B is the difference between perturbative and non-perturbative vacuum.We have included the mass of the strange quark into the EoS and studied its effect on the overall properties of the strange quark star in this work.It is observed that the maximum mass reaches its highest value when.We have evaluated the range of the maximum mass of the strange quark star by solving the TOV equation for 57.55<B<91.54 MeV/fm^(3)necessary for stable strange quark matter at a zero external pressure condition with respect to neutrons.Maximum mass lies within the range of to when B ranges from 57.55 to 91.54MeV/fm^(3)and ms=0.It is noted that the maximum mass decreases with an increase in.Our model is found suitable for describing the mass of pulsars such as PSR J1614-2230 and Vela X-1 and the secondary objects in the GW170817 event.The model is also useful in predicting the radius of the recently observed pulsars PSR J0030+0451,PSR J0740+6620,and PSR J0952-0607 and the secondary objects in the GW170817 and GW190814 events.Our model is found to be stable with respect to all stability criteria of the stellar configurations and is also stable with respect to small perturbations.

The effects of strong magnetic fields and rotation on soliton stars at finite temperature

We study the effects of strong magnetic fields and uniform rotation on the properties of soliton stars in Lee-Wick model when a temperature dependence is introduced into this model. We first recall the properties of the Lee-Wick model and study the properties of soliton solutions, in particular, the stability condition, in terms of the parameters of the model and in terms of the number of fermions N inside the soliton (for very large N) in the presence of strong magnetic fields and uniform rotation. We also calculate the effects of gravity on the stability properties of the soliton stars in the simple approximation of coupling the Newtonian gravitational field to the energy density inside the soliton, treating this as constant throughout. Following Cottingham and Vinh Mau, we also make an analysis at finite temperature and show the possibility of a phase transition which leads to a model with parameters similar to those considered by Lee and his colleagues but in the presence of magnetic fields and rotation. More specifically, the effects of magnetic fields and rotation on the soliton mass and transition temperature are computed explicitly. We finally study the evolution on these magnetized and rotating soliton stars with the temperature from the early universe to the present time.

Magnetic Field Effect on β^＋ Decay in the Crusts of Accreting Neutron Stars

基于原子核的壳模型，高度的影响磁性在增大的中子星的外壳中在β ~ 上删除 +decay 被分析。~(54 ) 上的磁场效果 Mn 被讨论。结果显示出那一弱磁性成立在β ~+ 腐烂上做小效果但是一个强壮的磁场(B 】 10 ~(11 ) G ) 改进腐烂显然评估的β ~+ 。导出的结论将受益以后在原子天体物理学上开发进一步的研究。

Magnetic Effect Versus Thermal Effect on Quark Matter with a Running Coupling at Finite Densities

We investigate the quark matter in a strong magnetic field in the framework of SU(2) NJL model with a magnetic-field-dependent coupling. The spin polarization, the entropy per baryon, and the energy are studied by analyzing the competition of the magnetic effect and the thermal effect. The stronger magnetic field can enhance the spin polarization, arrange quarks in a uniform spin orientation, and change the energy per baryon drastically. However,it can hardly affect the entropy per baryon, which is dominated by the temperature. As the temperature increases, more quarks will be excited from the lowest Landau level up to higher Landau levels.

High Accuracy Calculation for Excited-State Energies of H Atoms in a Magnetic Field

<正> Using the recently developed finite-basis-set method with B splines,excited states of H atoms in a magneticfield have been calculated.Energy levels are presented for the ten excited states,2s_0,3d′_0,3p_0,3d_(-1),3d_(-1),4d_(-1),3d_(-2),4d_(-2),4f_(-2),and 5f_(-2) as a function of magnetic field strengths with a range from zero up to 2.35 × 10~6 T.The obtainedresults are compared with available high accuracy theoretical data reported in the literature and found to be in excellentagreement.The comparison also shows that the current method can produce energy levels with an accuracy higher thanthe existing high accuracy method [Phys.Rev.A 54 (1996) 287].Here high accuracy energy levels are for the first timereported for the 3d′_0,4d_(-1),4d_(-2),4f_(-2),and 5f_(-2) states.

Spontaneous magnetization of solid quark-cluster stars

Pulsar-like compact stars usually have strong magnetic fields, with strengths from -10^8 to -10^12 G on the surface. How such strong magnetic fields can be generated and maintained is still an unsolved problem,which is, in principle, related to the interior structure of compact stars, i.e., the equation of state of cold matter at supra-nuclear density. In this paper we are trying to solve the problem in the regime of solid quark-cluster stars.Inside quark-cluster stars, the extremely low ratio of number density of electrons to that of baryons ne /nb and the screening effect from quark-clusters could reduce the long-range Coulomb interaction between electrons to short-range interaction. In this case, Stoner＇s model could apply, and we find that the condition for ferromagnetism is consistent with that for the validity of Stoner＇s model. Under the screened Coulomb repulsion, the electrons inside the stars could be spontaneously magnetized and become ferromagnetic, and hence would contribute non-zero net magnetic momentum to the whole star. We conclude that, for most cases in solid quark-cluster stars, the amount of net magnetic momentum, which is proportional to the amount of unbalanced spins ξ =（n＋- n-）/ne and depends on the number density of electrons ne =n＋ ＋ n-, could be significant with non-zero ξ. The net magnetic moments of electron system in solid quark-cluster stars could be large enough to induce the observed magnetic fields for pulsars with B ~ 10^11 to ~ 10^13 G.

Landau quantization and spin polarization of cold magnetized quark matter

The magnetic field and density behaviors of various thermodynamic quantities of strange quark matter under compact star conditions are investigated in the framework of the thermodynamically self-consistent quasiparticle model.For individual species,a larger number density n_(i) leads to a larger magnetic field strength threshold that aligns all particles parallel or antiparallel to the magnetic field.Accordingly,in contrast to the finite baryon density effect which reduces the spin polarization of magnetized strange quark matter,the magnetic field effect leads to an enhancement of it.We also compute the sound velocity as a function of the baryon density and find the sound velocity shows an obvious oscillation with increasing density.Except for the oscillation,the sound velocity grows with increasing density,similar to the zero-magnetic field case,and approaches the conformal limit V_(s)^(2)=1/3 at high densities from below.

Nuclear Physics with Magnetic Charges

The magnetic spinor particles (magnetic charges) are the real structural components all varieties of the Mass, for example, atoms, nucleons, positrons and neutrinos. Atomic-shaped device of Mass is the natural and the only possible organization of electric and magnetic charges which can create a gravitational field. At level of a popular language one can define nucleons as “small atoms”, and positron and neutrino as “very small atoms”. The electric and magnetic fundamental particles in neutron and proton shells which by tradition should be called quarks have charges of smaller magnitude than the charges of particles in atomic shells. Positron which participates in the gravitational interaction and, consequently, has an atomic-shaped device is the most likely candidate for the role of the proton nucleus. The most likely candidate particles on the participation in nuclei of proton and neutron as well as in nuclei of the positron and neutrino are presented in the article. So-called abnormal magnetic moment of neutron is formed by the quark magnetic dipoles which are like to unpaired electrons in the so-called magnetic atoms rotate on the outer orbitals of the neutron shell. The participation of the “magnetic electron” (magneton) in the neutrino core assumes the existence of the so-called anomalous magnetic moment and in the neutrino shell. The existence of real magnetic charges in the structures of the Mass draws our attention on such important problem as interaction between charges in the framework of electromagnetic dipoles such as and in which manifest the weak attraction. Weak interaction by its nature is electromagnetic. So-called electromagnetic interaction, manifested in pairs of homogeneous charges of opposite signs, is either electric or magnetic, but not electromagnetic. The explanation of the weak interaction in the marked pairs of charges is based on the author’s concept of the World Physical Triad and “Dark Energy”. Forces responsible for the interaction of the charges composing the electromagnetic dipoles correspond, conditionally of the weak charges of the particles which what assume mutual suppression of the influence of their fields on the Energo-medium and the formation of the weak “Dark energy”. Complex of magnetic particles, the quark magnetic dipoles and magneton by means of which the interconversion of a proton and a neutron is realized and maintained their constant number in the atomic nuclei can be called as magnetic meson. Namely, a processes of interconversion between a neutron and a proton which, as a rule, are not accompanied by secretions, created the illusion of neutron stability in atomic nuclei. The energy created by an exchange of magnetic mesons between neutron and proton can be a component of nuclear forces (strong interaction). Another effective and, most likely, the main component in the composition of the nuclear forces is the gravitational “Dark Energy”. Physics and structure of neutrinos presented in the paper suggest that the nature of these particles closer to the ideology of E. Majorana than P. Dirac’s.

Neutrino energy loss by electron capture in magnetic field at the crusts of neutron stars

Based on the p-f shell model, the effect of strong magnetic field on neutrino energy loss rates by electron capture is investigated. The calculations show that the magnetic field has only a slight effect on the neutrino energy loss rates in the range of 10^8-10^13 G on the surfaces of most neutron stars. But for some magnetars, the range of the magnetic field is 10^13-10^18 G, and the neutrino energy loss rates are greatly reduced, even by more than four orders of magnitude due to the strong magnetic field.

强磁场下中子星外壳层的Gamow-Teller跃迁电子俘获

以核素^55Co和^54Mn为例．讨论了强磁场下的中子星外壳层Gamow—Teller跃迁（G-T）电子俘获率．结果表明，对于大部分中子星，表面磁场（10^4～10^9T）对Cr-T跃迁电子俘获率的影响很小，对于超磁中子星．表面磁场（10^9～10^13T）使GT跃迁电子俘获率降低大约2—3个数量级．

超强磁场下简并电子气体的磁化

致密天体(白矮星和中子星)内部的电子气体是简并的费米系统,它们的零点费米动能远大于热运动动能.根据零点费米能与电子静止能的比较可区分为非相对论和相对论两种情况,按电子拉莫尔轨道动能与零点费米能的比较又可区分为强和超强两种外磁场作用情况.本文研究了电子费米系统在超强磁场作用下的磁化问题,发现在非相对论和相对论两种情况中的磁化都呈现出de Haas-van Alphen震荡效应,但微分磁化率难以大于临界值1,说明在超强磁场下的电子气体难以发生Condon磁相变,只有当电子占据刚好填满第一朗道量子能级时,微分磁化率才能大于一.