基于相对论简并费米气体模型的Chandrasekhar极限

利用简并费米统计理论,并考虑到电子运动的相对论效应,求出白矮星的极限质量—Chan- drasekhar极限质量,并进一步讨论了这一极限质量在恒星演化过程中的意义。

一类具扰动的Chandrasekhar H-方程的可积极小正解

讨论了迁移理论和气体动力学中一类具扰动的ＣｈａｎｄｒａｓｅｋｈａｒＨ方程：Ｈ（ｘ）＝φ（ｘ）＋λＨ（ｘ）∫ＧＫ（ｘ）Ｋ（ｘ）＋Ｋ（ｔ）Ｈ（ｔ）ｄｔ＋∫ＧＰ（ｘ，ｔ，Ｈ（ｘ），Ｈ（ｔ））ｄｔλ＞０式中，Ｇ是Ｒｎ中的紧集；φ（ｘ），Ｋ（ｘ），Ｐ（ｘ，ｔ，ｕ，ｖ）为已知函数；λ为常数．并得到了上述方程可积极小正解的存在性、逼近性、稳定性．

Chandrasekhar H-方程组的可积正解

把ＣｈａｎｄｒａｓｅｋｈａｒＨ方程推广到ＣｈａｎｄｒａｓｅｋｈａｒＨ方程组情形，得到了方程组适定的条件，并在此基础上研究了具有可积正解的必要充分条件和可积正解的稳定性，此外讨论了歧点．

正方形区域上Chandrasekhar方程D_4对称正解的计算

运用Liapunov-Schmidt约化和对称破缺分歧的方法,计算了正方形区域上Chan-drasekhar方程边值问题的D4对称的正解.

一类具扰动Chandrasekhar H-方程的可积正解

本文讨论了迁移理论和气体动力学中一类具扰动的 Ｃｈａｎｄｒａｓｅｋｈａｒ Ｈ－方程：这里Ｇ是Ｒ～ｎ中的有界闭集，为已知函数，λ为常数。本文研究并得到了方程（０．６）可积正解的存在性、个数、逼近性、稳定性，改进和发展了〔４〕［５］［７］的结果。

一类Chandrasekhar H—方程组的可积正解

本文把的Chandrasekhar H-方程推广到Chandrasekhar H-方程组情形,得到了方程组适定的条件,并在此基础上研究了具有可积正解的必要充分条件和稳定性。

Chandrasekhar方程之拉氏形式、Neother流及其反散射方程

文中给出了Chandrasckhar方程的拉氏形式,由此导出了三种类型的Neother守恒流并将此方程化为手征形式,进而给出其反散射方程。

Solvability of Chandrasekhar’s Quadratic Integral Equations in Banach Algebra

In this paper, we prove some results concerning the existence of solutions for some nonlinear functional-integral equations which contain various integral and functional equations that are considered in nonlinear analysis. Our considerations will be discussed in Banach algebra using a fixed point theorem instead of using the technique of measure of noncompactness. An important special case of that functional equation is Chandrasekhar’s integral equation which appears in radiative transfer, neutron transport and the kinetic theory of gases [1].

迁移理论中—类具扰动的Chandrasekhar方程解的存在性定理

本文对迁移理论中一类具扰动的Chandrasekhar方程在L[0.1]中解的存在性和逼近问题作了某些研究。本文结果改进和推广了文[1—6]中的某些结果。

The Creation of Neutron Stars and Black Stars and How the Chandrasekhar Limit Prevents the Creation of Intermediate Black Stars

Using a program written in Excel, it was found that a supernova remnant, with a mass between 1.44 and 2 solar masses, contracts down to a neutron star. During the collapse, the decreasing gravitational potential slows time. Here, the pressure becomes high enough to stop the contraction. At greater than 2.2 solar masses, while the remnant is still contracting, the gravitational potential causes time to relatively freeze at the center, and stop the contraction before the pressure gets high enough to stop it, as it did in a neutron star. This also freezes the flow of information concerning the decrease in gravitational potential, thus, the frozen portions remain frozen and do not contract down any further and become imaginary. On top of this frozen center, additional matter physically and relatively contracts and the radius of the freeze point moves out. If the freeze made its way to the surface, it would meet the condition of a black hole, having a Schwarzschild radius;but it does not quite get there. The surface is not quite frozen. Even though these “almost black holes” do not have an event horizon, they are almost as small as that described by the Schwarzschild radius and due to the gravitational red shift, are very hard to see. A black star has been created. A contracting white dwarf at the Chandrasekhar limit (1.44 solar masses) has a density of about 1 × 109 kg/m3. After it cools and then collapses into a neutron star, it will have a minimum density of 3.5 × 1015 kg/m3 near the surface. This article explains how these two densities relate to why there are no supernova created stellar black stars above 15 solar masses and why super massive black stars start at 50,000 solar masses? Extracting limits like these cannot be accomplished using the standard black hole model, but this black star model has revealed these size limits and a lot more.

Life Origin in the Milky Way Galaxy: III. Spatial Distribution of Overheated Stars in the Solar Neighborhood

A concept of ensemble averaged stellar reactors is developed to study the dynamics of processes occurring in stars, allocated in the ~200 pc solar neighborhood. According to the effective temperature value, four stellar classes are identified, for which the correlation coefficients and standard deviation are counted. The theory of the buoyancy terrestial elements is generalized to stellar systems. It was suggested that stars are over-heated due to the shift parameters of the nuclear processes occurring inside the stars, which leads to the synthesis of transuranium elements until the achievement of a critical nuclear mass and star explosion. The heavy transuranium elements sink downward and are concentrated in the stellar depth layers. The physical explanation of the existence of the critical Chandrasekhar star limit has been offered. Based on the spatial analysis of overheated stars, it was suggested that the withdrawal of the stellar reactor from the equilibrium state is a consequence of extragalactic compression inside the galaxy arm due to the arm spirality (not to be confused with the spirality of the galaxy itself).

美在科学创造中“孤独”绽放——纪念钱德拉塞卡诞辰100周年

美籍印度天体物理学家萨婆罗门扬·钱德拉塞卡（S．Chandrasekhar，1910～1995）“因为对恒星结构和演化过程的研究，特别是因为对白矮星的结构和极限质量的精确预言”而荣获1983年度诺贝尔物理学奖．作为20世纪最杰出的科学家之一，钱德拉塞卡以其在天体物理学、物理学和应用数学等领域广博的贡献闻名于世．在其充满创造传奇的一生中，

爱丁顿、钱德拉塞卡关于白矮星的争论及其启示

对爱丁顿、钱德拉塞卡关于白矮星的争论作了介绍,讨论了这场争论和钱德拉塞卡的科研风格带给我们的启示.

瑞利-泰勒不稳定性线性增长的密度梯度致稳

研究了密度梯度对瑞利-泰勒不稳定性的致稳作用,采用有限元算法求解钱得拉塞卡方程本征值问题,得到不同密度分布下理想不可压流体力学量的扰动线性增长率及扰动速度分布。扰动增长率结果与修正的Lindl公式的计算结果比较发现:扰动分布的峰值位于密度梯度标长的取值位置处,波长与密度标长可比拟时,扰动增长率显著偏离Lindl公式,而长波和短波极限情况下,数值解和Lindl公式符合较好。

Instability of binary nanofluids with magnetic field

The present paper investigates the effects of a vertical magnetic field on the double diffusive nanofluid convection, The effects of the Brownian motion and ther- mophoresis due to the presence of nanoparticles and the effects of the Dufour and Sorer parameters due to the presence of solute are included in the investigated model. The normal mode technique is used to solve the conservation equations. For the analytical study, valid approximations are made in the complex expression for the Rayleigh number to get useful and interesting results. The bottom heavy binary nanofluids are more stable than the regular binary fluids, while the top heavy binary nanofluids are less stable than the regular binary fluids. The critical wave number and the critical Rayleigh number in- crease whereas the frequency of oscillation （for the bottom heavy configuration） decreases when the Chandrasekhar number increases. The numerical results for the alumina-water nanofiuid are studied by use of the MATHEMATICA software.

IBM用植物制造环境友好的塑料

IBM研究员3月9日称，他们已经发明了一种用植物制造环境友好塑料的方法。它们可以取代石油基的对环境不友好的产品。据IBM公司在北加州的Almaden研究中心科技部经理Chandrasekhar“Spike”Naraya透露，这项突破有可能用节能的方法生产生物降解塑料。

线上高端摩托车出租平台WickedRide完成150万美元新一轮融资

据外媒消息,线上高端摩托车出租平台WickedRide宣布完成了一笔150万美元的新一轮融资,投资方为Sutures India主席Chandrasekhar Gopalan的家族投资基金。根据消息人士透露,本轮融资的估值可能达到了1000-1080万美元。

中子星的形成机理在固体物理教学中的应用

本文在固体物理学关于电子色散关系和态密度讨论的基础上,研究了其电子在相对论和非相对论下色散关系的区别,正是这种区别导致了超大质量天体最终演化出现截然不同的结果.该理论推导过程可以与固体物理学中电子行为的研究紧密联系起来,将之引入到固体物理的教学中,不仅可以加深学生对固体中电子行为的认识,还能拓展学生的知识,让其对电子的相对论行为有一定的认识.