等离子体与“太阳风”漫谈

 一、物质的第四态--等离子体我们知道,物质通常处于三种聚集态,即固态、液态和气态,随着温度的变化,物质的三态之间可以互相转化。如果温度升高到104K甚至105K,分子间和原子间的运动十分剧烈,彼此间已难以束缚,原子中的电子因具有相当大的动能而摆脱原子核对它的束缚,成为自由电子,原子失去电子变成带正电的离子。这样,物质就变成了一团由电子和带正电的离子组成的混合物。发生了电离的气体,无论是部分电离还是完全电离,虽然描述普通气体的密度、温度、压强等仍适用,但它的主要性质已发生了本质的变化。在气体中电离成分只要超过1‰,它的行为就主要由电子和离子间的库仑力来支配。     

漫谈自然之“声”

 人们对声音是再熟悉不过的了,每时每刻都要与声音打交道。从大自然的风声、雷声,到飞机划破长空的呼啸声;从婴儿“呱呱”落地时的第一声哭泣,再到人类用于交流的语言和美妙的音乐,声音与人类总是相伴的。没有声音的世界将是不可思议、极其恐怖、无法生存的。那么,什么是声音?其奥秘何在?这就让我们走进声音的世界,揭开其神秘的面纱。一、声音的物理机制平时人们所说的声音,从物理上讲,指的就是声波,声波本质上是一种机械纵波。     

雕塑“物之道”

 2001年6月上旬,在中国美术馆举办的《艺术与科学国际作品展暨学术研讨会》上,展出了一座高约48米名为“物之道”的金属雕塑。该雕塑的创作者、清华大学美术学院副研究员卢新华介绍,这个雕塑是由著名物理学家李政道创意,在中科院院长路甬祥及许多科学家的指导下完成的。雕塑在创作中运用点、线、面运动变化所具有的丰富内涵和表现力,以线的单纯、简洁的视觉效果来表达正负电子对撞的科学技术特征,用一根不断延伸的线在同一圆心做涡旋运动,并使线的两端为两个极点的形态,向外延伸表现出“至大无极”,向内回归意味着“至小无内”。     

计算机的“快”与“大”

 1946年第一台真空管电子数字计算机问世,当时主要用于数值计算。50余年以来,计算机技术发展迅速,从用于数值计算到今天可以处理各种形式的信息,极大地推动了信息技术的发展。现代信息技术是以数字计算机为基础的。几十年来,数字计算机的发展,始终围绕着两个基本问题,这就是“快”和“大”。所谓“快”,就是运算速度快;所谓“大”,就是存储器的容量大。回顾人类历史的发展,信息技术的进步与发展起着十分重要的作用。过去人类以符号、图形、图画、声音、语言、文字等模拟量记录信息,传递信息。随着人类社会的进步,产生的信息越来越多。人们用信息爆炸来形容当前信息的数量和产生的速度。     

计算机的“聪明”与“笨”

 计算机聪明吗?你一定会觉得这还用问!现在几乎什么事情都离不开计算机,它几乎什么事情都能干,而且比人干得快、干得好。日常生活、文化娱乐、行政事业管理,工厂、企业、银行、金融业的运营,公安交通管理,案件侦破、医疗卫生、科学技术的研究开发等等,几乎样样都离不开计算机。随随便便就可以举出很多例子。用计算机写文章比手写要方便得多,写错了,不合适,很容易修改;到超市买东西,选了一大筐,收银员一下子就把账结清,还打出一张收据,比手工结算快多了;照的照片不理想,计算机可以修改,老照片可以复原,模糊的照片可以变清晰.     

“电势”“电势差”的教学设计

 设计思想物理知识与一般的文化知识存在着密切的联系,在教学中如能把物理概念整合到更广阔的文化背景中,就能使学生更深刻地理解这一概念。在本节课的教学中,通过对包含“势”字的词语的讨论,使学生理解“势”的一般含义,这样有利于学生深刻理解电势概念。类比是人类研究、理解未知事物的一种有效而常用的方法。学生对重力场中“地势”的概念、水流从“地势”高处流到“地势”低处的现象及重力做功跟始末位置的“地势差”有关的规律有直观的印象。所以从“地势”概念出发,通过类比建立电势概念,是一种易于理解而直观的方法。     

“光”有“重量”吗?

 四百年前,伽利略曾利用实验深入地研究了落体和抛体的运动.后来,从盛传的比萨斜塔实验中,人们发现任何物体的惯性质量m_I都等于引力质量m_G.大约80年前,上述发现又成了广义相对论的基本出发点--等效原理.爱因斯坦还告诉我们,光子在引力场中也遵循这一原理.     

相对论中的“观测”与“看到”有何不同

 1905年爱因斯坦发表了狭义相对论,其时空观之一就是“运动的尺缩短”。接受相对论的所有人都相信这种尺缩现象是可以用眼睛看到或用照相机拍摄到的。一个运动物体看起来将沿运动方向缩短为原来的1-β2倍β=ｖｃ,ｖ是物体运动的速度大小,ｃ是光速,坐在高速飞船中的人从窗外看出去时,将看见球形物体缩成一个椭球体这些说法好像都是无可非议的。这种观念一直持续了54年之久,直到1959年美国物理学家戴勒尔发表了一篇文章,认为这种观念是错误的,他纠正了存在于所有人中间的这个偏见。提出“尺缩”现象可以“观测”或者“测量”,却不能用眼“看到”。     

盘古开天“大爆炸”

 我国有个非常美丽的神话,说的是一个叫盘古氏的人开天辟地的故事.在天地还没有形成的遥远的古代,如今的宇宙在当时是一片混沌,没有上下左右,也没有东南西北,就像个浑圆的鸡蛋.在这个“鸡蛋”的中心.     

关于“数字地球”

 “数字地球”(The Digital Earth)最早提出于1997年下半年,1998年1月31日,美国副总统戈尔在美国加利福尼亚科学中心发表了题为“数字地球:21世纪认识地球的方式”的讲演.     

介质效应对中子星性质的影响

用Bonn势和包含介质修正的相对论平均场模型讨论了介质效应对中子星性质的影响,结果表明BR标度参数的增加导致中子星质量及半径的增加.     

Nuclear Forces and Neutron Stars

Earlier work on nuclear forces is applied to astudy of cooled massive neutron stars. Nuclear forcesinside these stars cannot be neglected and theirinfluence on neutron star states is considered. One important property of nuclear forces is theirability to be repulsive, which results in the phenomenonof nuclear saturation. It is shown that this propertycan provide the balance of gravitational and nuclear forces in cooled massive neutronstars.     

The Effect of Hyperon-Hyperon Interaction on Neutron Stars

The equations ofstate of the neutron star matter are calculated in the relativistic mean-field approximation witl different hyperon coupling constants. The properties of neutron stars are studied by solving the OppenheimerVolkoff equation. It manifests the properties of neutron stars - change explicitly as different hyperon coupling constants are concerned.``     

The Effect of Hyperon-Hyperon Interaction on Neutron Stars

The equations of state of the neutron star matter are calculated in the relativistic mean-field approximation with different hyperon coupling constants. The properties of neutron stars are studied by solving the Oppenheimer-Volkoff equation. It manifests the properties of neutron stars — change explicitly as different hyperon coupling constants are concerned.     

Neutrino Emission and Cooling of Dark-Matter-Admixed Neutron Stars

The GW170817 binary neutron star merger event in 2017 has raised great interest in the theoretical research f neutron stars. The structure and cooling properties of dark-matter-admixed neutron stars are studied here using relativistic mean field theory and cooling theories. The non-self-annihilating dark matter(DM) component is assumed to be ideal fermions, among which the weak interaction is considered. The results show that pulsars J1614-2230, J0348+0432 and EXO 0748-676 may all contain DM with the particle mass of 0.2–0.4 GeV. However,it is found that the effect of DM on neutron star cooling is complicated. Light DM particles favor the fast cooling of neutron stars, and the case is converse for middle massive DM. However, high massive DM particles, around1.0 GeV, make the low mass(around solar mass) neutron star still undergo direct Urca process of nucleons at the core, which leads the DM-admixed stars cool much more quickly than the normal neutron star, and cannot support the direct Urca process with a mass lower than 1.1 times solar mass. Thus, we may conjecture that if small(around solar mass) and super cold(at least surface temperature 5–10 times lower than that of the usual observed data) pulsars are observed, then the star may contain fermionic DM with weak self-interaction.     

Oscillations of Short Periods in Neutron and Strange Stars

We present a model of a remnant of supernova, and we analyze the correlation with the observational data to short periods oscillations between a neutron star and a strange matter star. The results confirm previous conclusions.     

Effects of Gravitational Correction on Neutron Stars with Antikaon Condensation

Effects of gravitational correction through the introduction of U bosons on neutron stars with antikaon condensation are studied in the relativistic mean field theory. How the global properties of neutron stars, redshift and the momentum of inertia are modified by gravitational correction and antikaon condensation are discussed here. Results show that antikaon condensation can occur at the core of pulsar PSR J1614-2230. Gravitational correction and antikaon condensation influence each other, and when coupling constant of U bosons and baryons becomes very high, effects of antikaon condensation almost vanish. Moreover, both the redshift and the momentum of inertia of neutron stars are sensitive to the constant of U bosons. Combining with observation data, we can provide a further constraint on coupling constant of U bosons.     

Influence of Interactions on Populations for Hyperons in Neutron Stars

The numerical results of the populations for the baryon octet in neutron star matter have been presented by solving a set transcendental equations in the framework of the relativistic mean field approximation. The influence of the hyperon interactions on hyperon populations in neutron star matter is discussed. The results manifest that when the ratio of the hyperon-to-nucleon couplings increases, all hyperons appear towards low baryon density direction.